ABSTRACT
We present radial velocities and chemical abundance ratios of [Fe/H], [O/Fe], [Si/Fe], and [Ca/Fe] for 264 red giant branch stars in three Galactic bulge off-axis fields located near (l, b) = (−5.5, −7), (−4, −9), and (+8.5, +9). The results are based on equivalent width and spectrum synthesis analyses of moderate resolution (R ≈ 18,000), high signal-to-noise ratio (S/N ∼ 75–300 pixel-1) spectra obtained with the Hydra spectrographs on the Blanco 4 m and WIYN 3.5 m telescopes. The targets were selected from the blue side of the giant branch to avoid cool stars that would be strongly affected by CN and TiO; however, a comparison of the color–metallicity distribution in literature samples suggests that our selection of bluer targets should not present a significant bias against metal-rich stars. We find a full range in metallicity that spans [Fe/H] ≈−1.5 to +0.5, and that, in accordance with the previously observed minor-axis vertical metallicity gradient, the median [Fe/H] also declines with increasing Galactic latitude in off-axis fields. The off-axis vertical [Fe/H] gradient in the southern bulge is estimated to be ∼0.4 dex kpc-1; however, comparison with the minor-axis data suggests that a strong radial gradient does not exist. The (+8.5, +9) field exhibits a higher than expected metallicity, with a median [Fe/H] = −0.23, that might be related to a stronger presence of the X-shaped bulge structure along that line-of-sight. This could also be the cause of an anomalous increase in the median radial velocity for intermediate metallicity stars in the (+8.5, +9) field. However, the overall radial velocity and dispersion for each field are in good agreement with recent surveys and bulge models. All fields exhibit an identical, strong decrease in velocity dispersion with increasing metallicity that is consistent with observations in similar minor-axis outer bulge fields. Additionally, the [O/Fe], [Si/Fe], and [Ca/Fe] versus [Fe/H] trends are identical among our three fields, and are in good agreement with past bulge studies. We find that stars with [Fe/H] ≲ −0.5 are α-enhanced, and that the [α/Fe] ratios decline at higher metallicity. At [Fe/H] ≲ 0, the α-element trends are indistinguishable from the halo and thick disk, and the variations in the behavior of individual α-elements are consistent with production in massive stars and a rapid bulge formation timescale.
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1. INTRODUCTION
Although the minor-axis of the Galactic bulge has been the subject of extensive high resolution spectroscopic study (e.g., Zoccali et al. 2008), there has been relatively little chemical characterization of stars in off-axis bulge fields. Iron and α-element abundances are reported by Gonzalez et al. (2011) in a field near the globular cluster NGC 6553 (l, b) = (+5.25, −3), but that is the only off-axis field for which significant (N ≳ 100 stars) chemical abundance data are presently available.9 Overall, the radial variation in [Fe/H]10 and [α/Fe] along the bulge major-axis and off-axis is poorly constrained.
It is also clear that the bulge is spatially complex, and a deep understanding will require a full three-dimensional sampling of the structure. McWilliam & Zoccali (2010) found red clump giants to be spatially distributed in an X-shaped structure that spans the inner ∼8°, and was confirmed in a density analysis by Saito et al. (2011). The metal-rich subset of the bulge appears to be predominant in the X-shaped structure (Ness et al. 2012; Uttenthaler et al. 2012; but see also de Propris et al. 2011).
Connected with these issues is the question of whether there is kinematic substructure in the bulge, and whether the population is comprised of multiple components. Some evidence suggests the bulge may host two dominant populations (Babusiaux et al. 2010; Bensby et al. 2011; Hill et al. 2011; Uttenthaler et al. 2012). At the most basic level, such a bimodality might be expressed in the bar and the "classical" bulge. Soto et al. (2007) argued that the metal-rich bulge stars exhibit a vertex deviation expected for stars orbiting in the bar, while the metal-poor ([Fe/H] <−0.5) stars could plausibly be on non-barred orbits. Hill et al. (2011) argue strongly for bimodality, connecting two putative peaks in the [Fe/H] distribution with differing [Mg/Fe] ratios. Bensby et al. (2011) also find evidence for bimodality in their sample of 26 microlensed bulge dwarfs and subgiants, although they have recently increased their sample to 58 stars (Bensby et al. 2013) and now favor a multi-component model that may also incorporate the bimodal structures found in previous studies. Similarly, Ness et al. (2013), using [Fe/H] values derived from moderate resolution spectra of a large sample (∼28,000) of bulge giant and clump stars, deconvolve the metallicity distributions into five separate Gaussians that are asserted to vary systematically with Galactic latitude and longitude, and to reflect different populations. The BRAVA survey of ∼10,000 bulge M giants (e.g., Rich et al. 2007b; Kunder et al. 2012) does not find any hint of kinematic substructure or a significant classical bulge. Shen et al. (2010) argue that very strong limits are placed on any classical bulge fraction (≲8%–15% of the disk mass) from the BRAVA survey. It has been shown to be theoretically possible for a rapidly rotating bar to spin up a classical bulge (e.g., Shen et al. 2010; Saha et al. 2012), but such an effect would likely be unveiled by the metal-poor stars exhibiting rapid rotation and bar-like kinematics, which is not observed.
The question of correlations between [Fe/H], velocity, and/or velocity dispersion are among the most actively debated aspects of the substructure argument. Babusiaux et al. (2010) find a striking trend for the more metal-rich stars to have the highest velocity dispersion in Baade's Window (b = −4°); the trend reverses itself by b = −12°. Exploring intermediate minor-axis fields near b = −8° and −10°, Johnson et al. (2011) and Uttenthaler et al. (2012) find the common trend (e.g., Rich 1990) of velocity dispersion decreasing with increasing metallicity.
A further motivation to explore off-axis bulge fields addresses similarities and differences between such fields and the Galactic thick disk. In a bulge formation scenario in which the bar has thickened from a preexisting massive disk, it would not be surprising to find chemical similarities between bulge and thick disk stars; these might even be expected to predominate off-axis. Here, there is also some uncertainty. While early analyses (Zoccali et al. 2006; Fulbright et al. 2007; Lecureur et al. 2007) found that bulge stars were likely α-enhanced, particularly in their [O/Fe] and [Mg/Fe] ratios, compared to the thick disk, more recent differential studies (e.g., Meléndez et al. 2008; Ryde et al. 2010; Alves-Brito et al. 2010; Gonzalez et al. 2011) have instead concluded that the thick disk and metal-poor bulge likely share identical [α/Fe] distributions (but see also Bensby et al. 2013). However, it is not yet clear if these abundance similarities extend to super-solar metallicities and/or light odd-Z and heavy neutron-capture elements (e.g., Fulbright et al. 2007; Lecureur et al. 2007; Alves-Brito et al. 2010; McWilliam et al. 2010; Johnson et al. 2012).
Exploring the bulge in new fields, and near the bulge/halo boundary, offers significant opportunities to search for bulge substructure and to explore whether the bulge population is complex and multimodal over its whole volume. Although future samples will reach thousands of stars, our sample of 264 red giant branch (RGB) stars observed in multiobject mode at moderate (R ∼ 18,000) resolution will yield new constraints on the structure and substructure of the bulge. These data will also provide new tests of whether the bulge resembles the thick disk, and the presence of kinematic or composition substructure.
2. OBSERVATIONS AND DATA REDUCTION
The observations for this project were obtained between 2011 August 19–20 with the WIYN 3.5 m telescope at Kitt Peak National Observatory and 2011 September 8–12 with the Blanco 4 m telescope at Cerro Tololo Inter-American Observatory. WIYN was used to observe the northern bulge field centered near (l, b) = (+8.5, +9) and Blanco was used to observe the two southern bulge fields centered near (l, b) = (−5.5, −7) and (−4, −9). All spectra were acquired using the Hydra multifiber positioners and bench spectrographs. For WIYN–Hydra, we used the red fibers, 316 line mm-1 Echelle grating, red camera, and X18 filter to achieve a resolving power of R(λ/Δλ) ≈ 18,000. We also employed only one spectrograph setup with wavelength coverage ranging from about 6050–6350 Å. For Blanco–Hydra, we used the large 300 μm (2'') fibers, 400 mm Bench Schmidt camera, 316 line mm-1 Echelle grating, and the E6257 and E6757 filters to achieve R ≈ 18,000 in the first setup (6125–6345 Å) and R ≈ 15,000 in the second setup (6550–6840 Å). A summary of the observation dates, instrument setups, and exposure times for each field is provided in Table 1.
Table 1. Summary of Hydra Observations
| UT Date | Telescope | Setup | Exposure | Field (l, b) |
|---|---|---|---|---|
| 2011 Aug 19 | WIYN | 6250 | 3 × 3600 s | (+8.5, +9) |
| 2011 Aug 20 | WIYN | 6250 | 3 × 3600 s | (+8.5, +9) |
| 2011 Sep 8 | Blanco | 6700 | 3 × 3600 s | (−5.5, −7) |
| 2011 Sep 9 | Blanco | 6250 | 1 × 2700 s | (−5.5, −7) |
| 2011 Sep 10 | Blanco | 6250 | 4 × 3600 s | (−5.5, −7) |
| 2011 Sep 11 | Blanco | 6700 | 3 × 3600 s | (−4, −9) |
| 2011 Sep 11 | Blanco | 6250 | 1 × 3600 s | (−4, −9) |
| 2011 Sep 12 | Blanco | 6250 | 4 × 3600 s | (−4, −9) |
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The data reduction for both WIYN–Hydra and Blanco–Hydra data were carried out using standard IRAF tasks.11 Overscan removal and bias subtraction were accomplished using the ccdproc routine. The remaining data reduction tasks, which include fiber identification and tracing, scattered light removal, flat-field correction, ThAr wavelength calibration, cosmic-ray removal, sky subtraction, and object spectrum extraction, were carried out using the dohydra task. For the spectrograph setups that included the ∼6275–6330 Å telluric absorption feature, we observed several rapidly rotating B stars at various airmasses in order to remove telluric contamination in the object spectra. The final telluric correction was applied with the telluric IRAF task. All spectra were then combined via co-addition and continuum normalized by fitting a low order polynomial through the continuum points identified in Fulbright et al. (2006; their Table 5). The signal-to-noise ratio (S/N) of the combined spectra ranged from 75 to more than 300.
2.1. Target Selection
Since many of the previous bulge spectroscopic analyses have focused primarily on minor-axis fields (see Section 1), we targeted fields that were located away from the minor-axis (i.e., l ≠ 0). The observed fields were also selected to have relatively low interstellar extinction (E(B − V) ≲ 0.35), in order to minimize the integration time needed to reach S/N ≳ 75. For the Blanco, 5 hr of integration with our Hydra setups yields S/N ≳ 75 for stars with V ≲ 14.5. Given the higher airmass and shorter time frame with which we were able to observe the bulge with WIYN, we selected brighter targets (V ≲ 13.5–14). However, the significant throughput increase provided by the recent upgrade to the WIYN bench spectrograph (Bershady et al. 2008; Knezek et al. 2010) proved to make the selection of brighter stars an unnecessary constraint.
Unfortunately, constraining bulge membership for individual stars is often a difficult task using currently available data. Although high-quality optical photometry is not available for large regions of the bulge, the 2MASS database (Skrutskie et al. 2006) provides accurate coordinates and infrared photometry for the bright giants we were targeting. From the raw 2MASS catalog, we created an initial target list by only selecting stars which had: (1) 4000 K < Teff < 4800 K, (2) V < 14.5, and (3) log(g) < 2.5. The temperatures were determined using the J−K color–temperature relation provided by Alonso et al. (1999, 2001). All stars were individually dereddened using the E(B − V) values derived from the Schlegel et al. (1998) dust maps. Optical V magnitudes were estimated by taking the Teff values calculated from J−K and then inverting the Alonso et al. (1999) V−K color–temperature relation to solve for V. The range of possible log(g) values for each star were determined by examining the temperature–gravity–color relations in Kučinskas et al. (2005, 2006) to ensure log(g) < 2.5.12 The culled preliminary target list of ∼1000–3000 stars was then input into the Hydra fiber positioning software to produce an optimal configuration file for each field. In addition to ∼10–20 sky fibers for each configuration, we were able to place fibers on 91 stars for the (−5.5, −7) field, 105 stars for the (−4, −9) field, and 68 stars for the (+8.5, +9) field.
In Figure 1 we show 2MASS color–magnitude diagrams (CMDs) for all three fields, and also identify the observed target stars. While ∼90% of the targets in the two southern bulge fields and all of the stars in the northern bulge field lie well on the bulge RGB, ∼10% of the stars in the two southern bulge fields lie in a region that is likely a mix of bulge RGB and foreground red clump stars (the approximate separation is illustrated by the dashed blue lines in Figure 1). It is possible that some of these targets are actually foreground red clump stars, but we find only a small fraction of the bluest stars to have large proper motions and estimate the contamination ratio to be ≲10% of the total sample (see Section 4.1.1). For the majority of target stars that lie on the RGB, it is clear from Figure 1 that the observations are biased toward the bluer side of the RGB. This is a result of our choice to not select stars with Teff < 4000 K, in order to avoid strong CN and TiO molecular features in the spectra that would prevent reliable abundance determinations via equivalent width measurements. However, we show in Section 4.1.1 that we do not expect the selection of bluer stars to produce a strong metallicity bias.
Figure 1. KS vs. J − KS color–magnitude diagrams for the three observed bulge fields. The small black circles are point sources from the 2MASS catalog, and the filled red circles are the stars observed in the (l, b) = (−5
5, −7°), (−4°, −9°), and (+85, +9°) fields. The dashed blue lines designate the approximate separation between the bulge RGB and the foreground red clump population.
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Standard image High-resolution image3. DATA ANALYSIS
3.1. Model Stellar Atmospheres
As mentioned above, we used the dereddened (J − KS)o color13 for each star to derive Teff via the Alonso et al. (1999) color–temperature relation. In order to account for interstellar extinction, we assumed the relation E(J − KS)/E(B − V) = 0.505 (Fiorucci & Munari 2003) and used the recommended E(B − V) value from Schlegel et al. (1998).14 The average E(B − V) values were 0.240 (σ = 0.036), 0.136 (σ = 0.008), and 0.385 (σ = 0.024) for the (−5.5, −7), (−4, −9), and (+8.5, +9) fields, respectively. We did not attempt to refine Teff using excitation equilibrium; however, a star-by-star examination of the log 
(Fe i) abundance versus excitation potential plot indicated that significant (≳100 K) Teff adjustments were likely not necessary. This was true even for the most metal-rich stars ([Fe/H] >+0.2), which fall just outside the calibration range of the Alonso et al. (1999) J−K color–temperature relation. In a more quantitative sense, the average, median, and standard deviations of the slopes for the log (Fe i) versus excitation potential plots were: −0.006, −0.011, and 0.043 for the (−5.5, −7) field, +0.002, −0.004, and 0.032 for the (−4, −9) field, and −0.019, −0.023, and 0.037 for the (+8.5, +9) field. For comparison, altering Teff ±100 K in a "typical" bulge giant with [Fe/H] = −0.3 is expected to produce a change in the magnitude of the slope by ∼0.04 at Teff = 4200 K and ∼0.02 at Teff = 4800 K.
Surface gravities were derived by interpolating within the 11 Gyr isochrones provided by the Dartmouth Stellar Evolution Database (Dotter et al. 2007).15 We initially assumed a level of α-enhancement that followed the [α/Fe] versus [Fe/H] trends of Gonzalez et al. (2011) and Johnson et al. (2011). However, after measuring [α/Fe] for each star we reinterpolated using a grid with the appropriate level of α-enhancement. As can be seen in Figure 2, our assumed log(g) values are typically in good agreement with other log(g) estimates of bulge RGB stars in the literature. Note that the literature values shown in Figure 2 represent a variety of techniques for deriving log(g), including ionization equilibrium, isochrone fitting, and photometric estimates.
Figure 2. The four panels show the relationship between log(g) and Teff for bulge RGB stars in our combined sample (filled gray circles) and those available in the literature (filled blue circles). Each panel contains only stars within the listed metallicity range. A 3rd order polynomial is fit to the literature data and is illustrated by the solid blue lines. The literature data are from: McWilliam & Rich (1994), Rich & Origlia (2005), Fulbright et al. (2006), Lecureur et al. (2007), Rich et al. (2007a), Meléndez et al. (2008), Zoccali et al. (2008), Alves-Brito et al. (2010), Ryde et al. (2010), Johnson et al. (2011), and Rich et al. (2012).
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Standard image High-resolution imageFor each star the model atmosphere metallicity was set at [M/H] = −0.3 and then adjusted to equal the average derived [Fe/H] ratio. Similarly, the microturbulence (vt) was set at 2 km s-1 and then adjusted so that the plot of Fe i abundance versus line strength produced a zero slope. For all stars the model atmosphere was calculated by interpolating within the α-rich AODFNEW ATLAS9 grid (Castelli et al. 1997).16 While not all of the stars in our sample are α-rich, Fulbright et al. (2007) found that the impact of using the solar scaled versus α-rich ATLAS9 models on derived abundances was relatively small for bulge giants (≲0.1 dex in most cases). Specifically, the average effect on [Fe/H], [O/Fe], [Si/Fe], and [Ca/Fe] was found to be (in the sense AODFNEW–ODFNEW): +0.06 (σ = 0.03), −0.05 (σ = 0.07), +0.02 (σ = 0.03), and −0.02 (σ = 0.03), respectively. We performed the same test on our data set and found that the average AODFNEW–ODFNEW abundance change for [Fe/H], [O/Fe], [Si/Fe], and [Ca/Fe] was similar at: +0.05 (σ = 0.07), +0.06 (σ = 0.06), +0.10 (σ = 0.03), and −0.10 (σ = 0.03), respectively. The final model atmosphere parameters, photometry, and E(B − V) values are provided in Table 2.
Table 2. Star Identifiers, Photometry, Model Atmosphere Parameters, and Radial Velocities
| Star ID | E(B − V) | J | H | KS | Teff | log(g) | [Fe/H] | Vt | RV Helio. |
|---|---|---|---|---|---|---|---|---|---|
| 2MASS | (K) | (cgs) | (km s-1) | (km s-1) | |||||
| (l, b) = (−5.5, −7) | |||||||||
| 18011989−3723462 | 0.212 | 10.996 | 10.313 | 10.148 | 4405 | 1.20 | −1.50 | 1.55 | +50.3 |
| 18003452−3729217 | 0.232 | 11.809 | 11.142 | 11.022 | 4605 | 1.60 | −1.40 | 2.15 | −78.2 |
| 18011692−3722508 | 0.222 | 11.436 | 10.753 | 10.608 | 4475 | 1.45 | −1.33 | 1.75 | +49.0 |
| 18005584−3739103 | 0.212 | 11.525 | 10.805 | 10.659 | 4360 | 1.30 | −1.31 | 1.80 | +171.3 |
| 18015010−3735279 | 0.196 | 11.568 | 10.880 | 10.736 | 4425 | 1.50 | −1.15 | 1.80 | −45.9 |
| 18005916−3727585 | 0.220 | 11.610 | 10.935 | 10.796 | 4510 | 1.70 | −1.04 | 1.55 | +227.8 |
| 18005027−3707505 | 0.268 | 11.908 | 11.261 | 11.110 | 4630 | 1.90 | −0.99 | 1.85 | +48.4 |
| 18005234−3715478 | 0.250 | 11.168 | 10.407 | 10.294 | 4395 | 1.55 | −0.99 | 1.40 | +49.2 |
| 18020106−3737561 | 0.203 | 11.266 | 10.568 | 10.416 | 4390 | 1.55 | −0.98 | 1.65 | +26.0 |
| 17595541−3713447 | 0.324 | 11.425 | 10.688 | 10.558 | 4520 | 1.75 | −0.90 | 1.45 | +39.7 |
| 17595664−3725304 | 0.268 | 12.034 | 11.318 | 11.220 | 4585 | 1.85 | −0.89 | 1.20 | −104.7 |
| 18021345−3730371 | 0.191 | 11.669 | 10.910 | 10.748 | 4200 | 1.35 | −0.80 | 1.90 | −42.4 |
| 17594241−3718247 | 0.311 | 11.436 | 10.669 | 10.529 | 4395 | 1.60 | −0.76 | 2.15 | −94.9 |
| 18013342−3726339 | 0.202 | 11.784 | 11.095 | 10.979 | 4505 | 1.75 | −0.76 | 1.90 | +0.5 |
| 18003204−3726008 | 0.243 | 10.558 | 9.755 | 9.587 | 4150 | 1.25 | −0.75 | 1.55 | −70.9 |
| 18013580−3740055 | 0.211 | 11.383 | 10.589 | 10.450 | 4195 | 1.35 | −0.75 | 1.80 | −192.4 |
| 18013799−3725131 | 0.201 | 11.349 | 10.591 | 10.412 | 4175 | 1.35 | −0.74 | 1.60 | +45.0 |
| 18022149−3713494 | 0.223 | 11.033 | 10.276 | 10.106 | 4225 | 1.40 | −0.71 | 1.75 | −18.9 |
| 18011408−3711299 | 0.237 | 12.001 | 11.310 | 11.203 | 4580 | 1.95 | −0.69 | 1.40 | +63.8 |
| 18021275−3737543 | 0.206 | 11.938 | 11.261 | 11.137 | 4525 | 1.85 | −0.67 | 1.45 | +36.9 |
| 17595027−3727293 | 0.265 | 11.679 | 10.864 | 10.744 | 4260 | 1.60 | −0.66 | 1.65 | −23.9 |
| 18002115−3715519 | 0.276 | 11.041 | 10.212 | 10.035 | 4115 | 1.30 | −0.61 | 1.55 | −158.9 |
| 17595366−3728186 | 0.266 | 11.857 | 11.216 | 11.019 | 4515 | 1.85 | −0.59 | 1.85 | −41.9 |
| 18001354−3709122 | 0.292 | 11.414 | 10.624 | 10.428 | 4175 | 1.50 | −0.58 | 1.65 | −101.9 |
| 18013960−3723398 | 0.211 | 11.616 | 10.847 | 10.669 | 4165 | 1.50 | −0.58 | 1.10 | −93.3 |
| 18021862−3734204 | 0.196 | 11.856 | 11.058 | 10.938 | 4210 | 1.55 | −0.57 | 1.55 | −30.0 |
| 18000535−3735315 | 0.226 | 10.115 | 9.348 | 9.163 | 4175 | 1.40 | −0.57 | 1.55 | −64.9 |
| 18013848−3721442 | 0.216 | 11.798 | 11.086 | 10.878 | 4230 | 1.55 | −0.55 | 1.70 | −78.5 |
| 17594792−3721422 | 0.316 | 10.871 | 10.128 | 9.954 | 4375 | 1.70 | −0.54 | 1.40 | −26.7 |
| 18011941−3721250 | 0.222 | 11.476 | 10.736 | 10.518 | 4155 | 1.45 | −0.54 | 2.00 | −231.8 |
| 18004824−3718074 | 0.251 | 11.531 | 10.714 | 10.539 | 4115 | 1.40 | −0.54 | 1.50 | −60.3 |
| 18014343−3708232 | 0.233 | 11.140 | 10.348 | 10.190 | 4185 | 1.50 | −0.54 | 1.35 | +22.8 |
| 18005852−3711524 | 0.252 | 11.873 | 11.260 | 11.065 | 4575 | 1.95 | −0.53 | 1.35 | −97.7 |
| 18020816−3714015 | 0.223 | 12.097 | 11.433 | 11.280 | 4505 | 1.85 | −0.53 | 1.60 | +41.4 |
| 18010932−3702079 | 0.262 | 11.050 | 10.291 | 10.065 | 4140 | 1.45 | −0.49 | 1.80 | +7.8 |
| 18010065−3740456 | 0.219 | 11.362 | 10.570 | 10.397 | 4135 | 1.45 | −0.49 | 1.55 | +4.2 |
| 17595640−3710383 | 0.326 | 10.761 | 9.998 | 9.836 | 4370 | 1.70 | −0.43 | 1.30 | +29.0 |
| 18012462−3738382 | 0.205 | 11.950 | 11.271 | 11.136 | 4485 | 1.85 | −0.43 | 1.90 | −74.6 |
| 18002880−3710171 | 0.274 | 11.899 | 11.253 | 11.098 | 4630 | 2.00 | −0.42 | 1.80 | +1.7 |
| 18024484−3714159 | 0.233 | 12.197 | 11.538 | 11.412 | 4615 | 2.00 | −0.42 | 1.35 | −3.8 |
| 18013206−3708133 | 0.235 | 12.106 | 11.451 | 11.322 | 4620 | 2.00 | −0.41 | 1.40 | −35.0 |
| 18004074−3740058 | 0.219 | 11.129 | 10.399 | 10.269 | 4385 | 1.75 | −0.36 | 1.80 | +27.5 |
| 18000013−3715053 | 0.297 | 11.412 | 10.663 | 10.486 | 4325 | 1.75 | −0.34 | 1.60 | +48.6 |
| 18015431−3717070 | 0.216 | 11.792 | 11.143 | 10.965 | 4470 | 1.90 | −0.34 | 1.30 | −139.9 |
| 18021006−3738193 | 0.206 | 11.920 | 11.261 | 11.161 | 4645 | 2.05 | −0.32 | 1.65 | −73.8 |
| 17595442−3721118 | 0.291 | 11.300 | 10.532 | 10.352 | 4265 | 1.60 | −0.29 | 1.60 | −51.2 |
| 18021721−3736096 | 0.202 | 11.735 | 11.078 | 10.962 | 4600 | 2.00 | −0.25 | 1.90 | −8.4 |
| 18005096−3733499 | 0.215 | 11.899 | 11.122 | 10.995 | 4270 | 1.70 | −0.25 | 1.25 | −74.1 |
| 18005923−3707111 | 0.262 | 11.534 | 10.744 | 10.575 | 4200 | 1.65 | −0.24 | 1.30 | −66.3 |
| 18011851−3706092 | 0.248 | 11.093 | 10.324 | 10.146 | 4210 | 1.65 | −0.24 | 1.65 | −67.1 |
| 18013395−3705551 | 0.236 | 10.910 | 10.147 | 9.954 | 4175 | 1.60 | −0.24 | 1.35 | −5.7 |
| 18022648−3728188 | 0.204 | 11.921 | 11.249 | 11.132 | 4555 | 1.95 | −0.20 | 1.95 | −98.1 |
| 18024919−3727234 | 0.215 | 11.553 | 10.958 | 10.772 | 4595 | 2.00 | −0.16 | 1.85 | +22.4 |
| 18023660−3716289 | 0.231 | 12.155 | 11.471 | 11.360 | 4580 | 1.95 | −0.14 | 1.90 | +45.6 |
| 17595509−3711099 | 0.326 | 10.786 | 10.066 | 9.871 | 4395 | 1.80 | −0.13 | 1.80 | −27.1 |
| 18005395−3731231 | 0.215 | 9.731 | 9.003 | 8.783 | 4165 | 1.60 | −0.13 | 1.90 | +17.3 |
| 18010322−3705447 | 0.264 | 12.067 | 11.444 | 11.276 | 4645 | 2.05 | −0.10 | 1.80 | +28.4 |
| 18014769−3739220 | 0.210 | 12.128 | 11.416 | 11.356 | 4615 | 2.00 | −0.10 | 1.20 | −197.7 |
| 17594807−3715283 | 0.335 | 11.520 | 10.793 | 10.662 | 4565 | 2.00 | −0.09 | 1.35 | −155.7 |
| 18013618−3706311 | 0.234 | 11.292 | 10.565 | 10.373 | 4260 | 1.70 | −0.07 | 1.50 | +150.7 |
| 18004314−3730156 | 0.222 | 11.892 | 11.223 | 11.074 | 4500 | 1.95 | −0.03 | 1.45 | −21.1 |
| 18014303−3740054 | 0.212 | 10.738 | 10.030 | 9.854 | 4315 | 1.75 | −0.03 | 1.75 | −32.6 |
| 18003751−3728200 | 0.232 | 10.465 | 9.657 | 9.490 | 4130 | 1.55 | −0.03 | 1.30 | −43.5 |
| 18011170−3727118 | 0.213 | 12.157 | 11.555 | 11.409 | 4690 | 2.05 | −0.01 | 1.85 | +7.1 |
| 18023846−3718345 | 0.228 | 11.903 | 11.175 | 11.008 | 4310 | 1.80 | −0.01 | 1.90 | −76.0 |
| 18011671−3722213 | 0.222 | 12.034 | 11.424 | 11.273 | 4665 | 2.05 | +0.00 | 1.60 | −53.6 |
| 18005985−3734507 | 0.208 | 11.526 | 10.762 | 10.590 | 4185 | 1.75 | +0.02 | 1.40 | −35.6 |
| 18000430−3711051 | 0.311 | 10.596 | 9.803 | 9.629 | 4245 | 1.70 | +0.06 | 1.60 | +79.2 |
| 18003552−3729476 | 0.226 | 11.270 | 10.506 | 10.376 | 4310 | 1.80 | +0.06 | 1.75 | −53.2 |
| 18001817−3732243 | 0.238 | 11.710 | 11.056 | 10.896 | 4535 | 1.95 | +0.08 | 1.35 | −32.6 |
| 18013039−3713086 | 0.234 | 11.301 | 10.574 | 10.374 | 4240 | 1.80 | +0.09 | 2.00 | −8.3 |
| 18012564−3741052 | 0.215 | 11.135 | 10.427 | 10.256 | 4330 | 1.85 | +0.10 | 1.90 | −57.1 |
| 18025713−3718318 | 0.233 | 9.999 | 9.250 | 9.049 | 4185 | 1.60 | +0.10 | 1.70 | +15.7 |
| 18011599−3741385 | 0.219 | 11.408 | 10.679 | 10.514 | 4300 | 1.80 | +0.11 | 1.50 | −9.3 |
| 18012944−3719488 | 0.225 | 12.181 | 11.576 | 11.419 | 4670 | 2.05 | +0.12 | 1.95 | −57.2 |
| 18020361−3719086 | 0.210 | 12.007 | 11.363 | 11.190 | 4485 | 1.95 | +0.15 | 1.90 | +6.5 |
| 18024024−3728187 | 0.208 | 11.803 | 11.088 | 10.870 | 4195 | 1.75 | +0.17 | 1.80 | +52.4 |
| 18000412−3717266 | 0.288 | 11.110 | 10.320 | 10.111 | 4145 | 1.70 | +0.17 | 1.70 | −52.9 |
| 18011177−3703344 | 0.270 | 10.829 | 10.123 | 9.895 | 4270 | 1.80 | +0.19 | 1.60 | −44.5 |
| 18001410−3725181 | 0.256 | 10.701 | 9.920 | 9.705 | 4110 | 1.65 | +0.19 | 1.40 | +22.5 |
| 18020300−3719418 | 0.205 | 10.172 | 9.420 | 9.222 | 4150 | 1.70 | +0.21 | 1.20 | +14.0 |
| 18004683−3703252 | 0.286 | 11.522 | 10.766 | 10.504 | 4100 | 1.65 | +0.22 | 1.50 | −92.0 |
| 18015404−3722564 | 0.201 | 10.959 | 10.260 | 10.059 | 4260 | 1.75 | +0.22 | 1.55 | −86.0 |
| 18013974−3704068 | 0.233 | 10.406 | 9.687 | 9.506 | 4305 | 1.80 | +0.27 | 1.60 | +85.0 |
| 18020704−3708064 | 0.226 | 11.494 | 10.860 | 10.688 | 4540 | 1.95 | +0.27 | 1.60 | −86.8 |
| 18023393−3730273 | 0.204 | 11.730 | 11.125 | 10.948 | 4575 | 2.00 | +0.33 | 1.90 | −24.3 |
| 18001720−3708374 | 0.292 | 10.695 | 9.928 | 9.676 | 4105 | 1.70 | +0.42 | 1.50 | −52.4 |
| 18003663−3708547 | 0.268 | 11.057 | 10.348 | 10.134 | 4295 | 1.80 | +0.42 | 1.40 | −1.5 |
| 18002569−3729578 | 0.240 | 11.855 | 11.251 | 11.030 | 4510 | 2.00 | +0.50 | 1.50 | −110.6 |
| 17594881−3716203 | 0.322 | 10.708 | 9.952 | 9.736 | 4250 | 1.85 | +0.59 | 1.45 | −79.3 |
| 18011201−3740090 | 0.209 | 11.423 | 10.789 | 10.621 | 4525 | 2.00 | +0.66 | 1.65 | −80.4 |
| (l, b) = (−4, −9) | |||||||||
| 18122552−3653049 | 0.139 | 11.527 | 10.906 | 10.775 | 4560 | 1.55 | −1.40 | 1.40 | −75.2 |
| 18120653−3654264 | 0.143 | 12.095 | 11.497 | 11.376 | 4660 | 1.65 | −1.38 | 1.00 | −48.6 |
| 18110179−3630394 | 0.138 | 12.165 | 11.540 | 11.418 | 4570 | 1.65 | −1.38 | 1.55 | −177.3 |
| 18124892−3626403 | 0.140 | 11.787 | 11.170 | 11.066 | 4650 | 1.75 | −1.33 | 1.50 | +87.4 |
| 18135164−3643463 | 0.119 | 12.266 | 11.615 | 11.532 | 4575 | 1.70 | −1.30 | 2.00 | −194.0 |
| 18124339−3635339 | 0.131 | 12.226 | 11.600 | 11.466 | 4525 | 1.65 | −1.28 | 1.55 | +82.0 |
| 18113921−3652069 | 0.134 | 11.927 | 11.269 | 11.114 | 4385 | 1.40 | −1.26 | 1.90 | +81.9 |
| 18111325−3646007 | 0.134 | 12.093 | 11.427 | 11.327 | 4510 | 1.65 | −1.21 | 1.40 | −191.8 |
| 18113833−3626322 | 0.146 | 11.951 | 11.219 | 11.077 | 4250 | 1.30 | −1.18 | 2.00 | −154.2 |
| 18111018−3639350 | 0.140 | 11.618 | 10.897 | 10.775 | 4320 | 1.35 | −1.16 | 1.40 | −184.0 |
| 18135243−3630481 | 0.123 | 11.896 | 11.285 | 11.154 | 4560 | 1.75 | −1.15 | 1.60 | −57.0 |
| 18121150−3627559 | 0.143 | 12.015 | 11.351 | 11.214 | 4430 | 1.60 | −1.10 | 1.50 | −101.7 |
| 18111963−3647245 | 0.134 | 11.955 | 11.279 | 11.138 | 4375 | 1.50 | −1.06 | 1.45 | −66.4 |
| 18140023−3635461 | 0.125 | 11.715 | 11.033 | 10.892 | 4345 | 1.50 | −1.05 | 1.80 | +144.4 |
| 18135881−3639345 | 0.128 | 11.376 | 10.692 | 10.555 | 4355 | 1.50 | −0.99 | 1.70 | −102.6 |
| 18121436−3654551 | 0.143 | 11.964 | 11.281 | 11.109 | 4290 | 1.50 | −0.93 | 1.75 | +67.0 |
| 18124228−3655079 | 0.138 | 11.062 | 10.336 | 10.178 | 4215 | 1.35 | −0.92 | 1.95 | +4.7 |
| 18122530−3637366 | 0.131 | 11.520 | 10.795 | 10.661 | 4265 | 1.50 | −0.89 | 1.60 | −4.8 |
| 18131370−3651584 | 0.129 | 11.994 | 11.321 | 11.189 | 4400 | 1.55 | −0.88 | 1.20 | −54.7 |
| 18134668−3623541 | 0.118 | 12.194 | 11.482 | 11.378 | 4355 | 1.60 | −0.88 | 1.80 | −0.5 |
| 18105081−3642137 | 0.135 | 11.853 | 11.227 | 11.098 | 4545 | 1.75 | −0.87 | 1.10 | −149.6 |
| 18124219−3631172 | 0.136 | 11.829 | 11.144 | 10.988 | 4315 | 1.55 | −0.87 | 1.60 | +30.8 |
| 18133688−3647054 | 0.125 | 11.510 | 10.860 | 10.739 | 4485 | 1.70 | −0.86 | 1.70 | −41.8 |
| 18123142−3639294 | 0.144 | 11.933 | 11.189 | 11.032 | 4185 | 1.45 | −0.80 | 1.75 | +255.1 |
| 18133038−3632229 | 0.131 | 12.339 | 11.734 | 11.621 | 4645 | 1.90 | −0.80 | 1.80 | −25.6 |
| 18133292−3624179 | 0.121 | 12.425 | 11.789 | 11.723 | 4675 | 1.95 | −0.78 | 2.00 | +27.7 |
| 18111681−3636318 | 0.139 | 9.774 | 9.033 | 8.866 | 4165 | 1.25 | −0.77 | 1.40 | +73.0 |
| 18105004−3640063 | 0.139 | 12.215 | 11.510 | 11.438 | 4490 | 1.70 | −0.76 | 1.80 | −106.6 |
| 18112334−3634194 | 0.139 | 11.853 | 11.216 | 11.072 | 4475 | 1.80 | −0.74 | 1.50 | +56.6 |
| 18131027−3632343 | 0.133 | 11.756 | 11.061 | 10.917 | 4320 | 1.60 | −0.73 | 1.60 | +103.3 |
| 18110293−3628041 | 0.139 | 11.708 | 11.001 | 10.823 | 4215 | 1.35 | −0.72 | 1.95 | +9.3 |
| 18132040−3623075 | 0.128 | 10.612 | 9.934 | 9.802 | 4385 | 1.70 | −0.71 | 1.65 | −68.2 |
| 18135588−3629188 | 0.120 | 11.675 | 11.027 | 10.896 | 4455 | 1.75 | −0.71 | 1.95 | −83.0 |
| 18105075−3635061 | 0.139 | 11.420 | 10.656 | 10.526 | 4195 | 1.40 | −0.70 | 1.40 | −56.2 |
| 18104188−3634541 | 0.141 | 11.795 | 11.139 | 11.067 | 4630 | 1.90 | −0.68 | 1.80 | −73.4 |
| 18132998−3628578 | 0.125 | 11.067 | 10.325 | 10.169 | 4170 | 1.40 | −0.68 | 1.85 | +27.6 |
| 18130544−3616563 | 0.136 | 12.015 | 11.309 | 11.145 | 4245 | 1.55 | −0.66 | 1.70 | −63.3 |
| 18115908−3654510 | 0.142 | 11.512 | 10.787 | 10.629 | 4225 | 1.50 | −0.64 | 1.35 | −124.5 |
| 18121077−3639094 | 0.135 | 12.089 | 11.423 | 11.245 | 4305 | 1.65 | −0.63 | 1.70 | −57.7 |
| 18120614−3629571 | 0.142 | 11.505 | 10.825 | 10.702 | 4425 | 1.75 | −0.58 | 1.35 | +29.0 |
| 18120213−3641599 | 0.141 | 11.866 | 11.297 | 11.126 | 4595 | 1.90 | −0.55 | 1.55 | −30.7 |
| 18123350−3654398 | 0.141 | 11.891 | 11.155 | 10.993 | 4185 | 1.55 | −0.54 | 1.70 | −96.9 |
| 18120973−3654184 | 0.143 | 11.594 | 10.887 | 10.663 | 4115 | 1.40 | −0.53 | 2.00 | −91.9 |
| 18105641−3632359 | 0.139 | 11.834 | 11.178 | 11.017 | 4380 | 1.70 | −0.52 | 1.55 | −269.5 |
| 18125106−3654091 | 0.134 | 11.873 | 11.257 | 11.135 | 4590 | 1.90 | −0.51 | 1.20 | +24.7 |
| 18111581−3648469 | 0.132 | 11.879 | 11.123 | 10.973 | 4160 | 1.55 | −0.51 | 1.40 | +106.2 |
| 18131387−3630130 | 0.132 | 12.065 | 11.373 | 11.201 | 4255 | 1.55 | −0.51 | 1.70 | −202.0 |
| 18123592−3634476 | 0.131 | 11.227 | 10.485 | 10.315 | 4145 | 1.55 | −0.50 | 1.85 | −139.1 |
| 18135736−3638266 | 0.129 | 12.042 | 11.379 | 11.178 | 4250 | 1.60 | −0.49 | 1.40 | −1.1 |
| 18133233−3626133 | 0.121 | 11.860 | 11.167 | 10.955 | 4145 | 1.55 | −0.49 | 1.60 | −207.5 |
| 18125003−3630269 | 0.137 | 12.146 | 11.496 | 11.343 | 4415 | 1.75 | −0.49 | 1.95 | −48.7 |
| 18130723−3618385 | 0.131 | 12.187 | 11.577 | 11.418 | 4500 | 1.80 | −0.45 | 1.60 | −53.2 |
| 18125800−3616427 | 0.138 | 12.427 | 11.791 | 11.716 | 4675 | 2.05 | −0.44 | 1.60 | +59.9 |
| 18111323−3637030 | 0.139 | 12.128 | 11.466 | 11.356 | 4500 | 1.80 | −0.44 | 1.30 | +7.6 |
| 18130427−3630012 | 0.135 | 12.363 | 11.842 | 11.637 | 4630 | 2.00 | −0.44 | 1.40 | +5.1 |
| 18124614−3617326 | 0.143 | 11.966 | 11.263 | 11.093 | 4250 | 1.60 | −0.43 | 1.70 | −36.3 |
| 18120399−3615387 | 0.156 | 11.779 | 11.018 | 10.891 | 4230 | 1.60 | −0.43 | 1.20 | −111.6 |
| 18123475−3624478 | 0.143 | 12.094 | 11.408 | 11.305 | 4460 | 1.85 | −0.43 | 1.80 | −104.4 |
| 18115661−3617533 | 0.156 | 12.210 | 11.564 | 11.459 | 4590 | 1.95 | −0.41 | 1.75 | +21.3 |
| 18113299−3623341 | 0.147 | 11.235 | 10.514 | 10.369 | 4270 | 1.65 | −0.40 | 1.35 | −64.8 |
| 18111553−3628156 | 0.139 | 11.035 | 10.342 | 10.147 | 4210 | 1.60 | −0.37 | 1.60 | −90.1 |
| 18125907−3644275 | 0.153 | 12.126 | 11.565 | 11.405 | 4670 | 2.05 | −0.37 | 1.90 | +6.9 |
| 18111726−3620302 | 0.143 | 12.174 | 11.509 | 11.364 | 4405 | 1.80 | −0.34 | 1.95 | −21.1 |
| 18111579−3625114 | 0.141 | 11.649 | 10.881 | 10.733 | 4145 | 1.55 | −0.34 | 1.25 | −6.3 |
| 18131305−3650449 | 0.128 | 11.938 | 11.356 | 11.169 | 4495 | 1.90 | −0.33 | 1.50 | −65.1 |
| 18123152−3636498 | 0.130 | 11.523 | 10.830 | 10.618 | 4160 | 1.60 | −0.33 | 1.40 | −5.4 |
| 18125914−3619208 | 0.140 | 11.864 | 11.262 | 11.097 | 4515 | 1.90 | −0.30 | 1.55 | −81.5 |
| 18115073−3650493 | 0.135 | 11.856 | 11.258 | 11.053 | 4410 | 1.80 | −0.29 | 2.10 | −70.8 |
| 18114648−3625169 | 0.150 | 12.413 | 11.796 | 11.698 | 4685 | 2.05 | −0.28 | 1.50 | −57.3 |
| 18113751−3629139 | 0.141 | 11.649 | 10.895 | 10.724 | 4130 | 1.60 | −0.28 | 1.30 | −52.0 |
| 18122243−3637539 | 0.133 | 11.362 | 10.715 | 10.546 | 4375 | 1.80 | −0.24 | 1.60 | +44.1 |
| 18133366−3644575 | 0.127 | 12.331 | 11.752 | 11.627 | 4680 | 2.05 | −0.23 | 1.70 | −79.5 |
| 18134702−3641477 | 0.126 | 12.083 | 11.512 | 11.376 | 4670 | 2.05 | −0.23 | 1.60 | +99.3 |
| 18125228−3618294 | 0.140 | 11.766 | 11.150 | 11.028 | 4600 | 1.95 | −0.21 | 1.65 | +7.6 |
| 18110942−3647198 | 0.133 | 12.288 | 11.702 | 11.573 | 4660 | 2.00 | −0.21 | 1.70 | −49.3 |
| 18104824−3638507 | 0.138 | 11.957 | 11.208 | 11.060 | 4185 | 1.60 | −0.19 | 1.20 | −224.2 |
| 18122301−3629462 | 0.137 | 10.311 | 9.598 | 9.392 | 4135 | 1.60 | −0.19 | 1.65 | +28.2 |
| 18133332−3645578 | 0.125 | 11.930 | 11.194 | 11.015 | 4130 | 1.60 | −0.18 | 1.70 | +23.5 |
| 18123434−3652241 | 0.137 | 10.907 | 10.251 | 10.081 | 4355 | 1.75 | −0.18 | 1.65 | −142.6 |
| 18112311−3625456 | 0.143 | 11.690 | 11.078 | 10.924 | 4525 | 1.95 | −0.17 | 2.00 | −0.9 |
| 18125463−3649277 | 0.137 | 11.588 | 10.938 | 10.756 | 4340 | 1.75 | −0.14 | 1.65 | −103.3 |
| 18123925−3620465 | 0.143 | 11.736 | 11.001 | 10.840 | 4195 | 1.65 | −0.14 | 1.30 | −177.4 |
| 18110629−3632146 | 0.137 | 10.483 | 9.850 | 9.628 | 4285 | 1.70 | −0.13 | 1.70 | +26.1 |
| 18133687−3639590 | 0.135 | 12.001 | 11.399 | 11.274 | 4625 | 2.00 | −0.11 | 1.90 | −81.2 |
| 18111505−3620576 | 0.142 | 11.836 | 11.238 | 11.097 | 4600 | 2.00 | −0.09 | 1.40 | −69.9 |
| 18120832−3628243 | 0.143 | 10.574 | 9.910 | 9.730 | 4320 | 1.75 | −0.09 | 1.55 | +39.9 |
| 18130815−3631460 | 0.133 | 10.652 | 9.901 | 9.723 | 4110 | 1.55 | −0.09 | 1.25 | −70.8 |
| 18120407−3636481 | 0.134 | 11.401 | 10.686 | 10.508 | 4190 | 1.65 | −0.09 | 1.40 | +82.4 |
| 18135786−3640300 | 0.128 | 11.801 | 11.147 | 10.948 | 4275 | 1.42 | −0.05 | 1.40 | −110.4 |
| 18131228−3619138 | 0.131 | 11.336 | 10.716 | 10.525 | 4385 | 1.80 | −0.04 | 1.65 | +2.7 |
| 18113372−3650200 | 0.134 | 11.714 | 11.085 | 10.835 | 4220 | 1.65 | −0.04 | 1.65 | +10.5 |
| 18115904−3650428 | 0.137 | 11.481 | 10.791 | 10.584 | 4185 | 1.65 | −0.01 | 1.40 | −24.8 |
| 18115448−3641161 | 0.139 | 11.705 | 11.047 | 10.904 | 4425 | 1.85 | −0.01 | 1.75 | −79.7 |
| 18123678−3649019 | 0.143 | 11.278 | 10.691 | 10.493 | 4470 | 1.85 | +0.02 | 1.30 | −104.1 |
| 18113965−3645408 | 0.135 | 11.884 | 11.193 | 11.032 | 4290 | 1.80 | +0.05 | 1.30 | −15.0 |
| 18135362−3636538 | 0.129 | 11.615 | 11.002 | 10.836 | 4465 | 2.00 | +0.06 | 1.85 | −69.2 |
| 18123168−3631555 | 0.133 | 12.427 | 11.801 | 11.705 | 4635 | 2.05 | +0.09 | 1.80 | +57.4 |
| 18115398−3623290 | 0.154 | 11.588 | 10.842 | 10.653 | 4120 | 1.70 | +0.09 | 1.60 | −96.1 |
| 18123393−3615508 | 0.149 | 11.863 | 11.301 | 11.133 | 4640 | 2.05 | +0.11 | 1.75 | −19.9 |
| 18120689−3643231 | 0.143 | 11.523 | 10.920 | 10.767 | 4555 | 2.00 | +0.11 | 1.80 | −70.7 |
| 18130482−3649019 | 0.135 | 11.849 | 11.118 | 10.935 | 4145 | 1.70 | +0.13 | 1.80 | −116.7 |
| 18110352−3646275 | 0.134 | 10.786 | 10.068 | 9.880 | 4160 | 1.60 | +0.14 | 1.50 | −77.8 |
| 18105013−3629557 | 0.143 | 10.701 | 10.026 | 9.868 | 4345 | 1.85 | +0.17 | 1.30 | +14.2 |
| 18121897−3630243 | 0.135 | 12.261 | 11.645 | 11.537 | 4635 | 2.05 | +0.22 | 1.50 | −28.7 |
| 18122029−3652333 | 0.139 | 10.984 | 10.385 | 10.190 | 4440 | 1.90 | +0.26 | 1.60 | −42.1 |
| (l, b) = (+8.5, +9) | |||||||||
| 17311256−1702018 | 0.359 | 10.392 | 9.555 | 9.385 | 4215 | 1.10 | −1.26 | 1.70 | +12.9 |
| 17290874−1632431 | 0.374 | 10.600 | 9.753 | 9.544 | 4125 | 0.95 | −1.23 | 1.90 | +35.7 |
| 17302885−1639588 | 0.390 | 10.855 | 10.048 | 9.824 | 4200 | 1.15 | −1.17 | 1.90 | −167.8 |
| 17304789−1623192 | 0.402 | 11.235 | 10.462 | 10.213 | 4235 | 1.20 | −1.14 | 1.80 | −211.7 |
| 17321080−1641479 | 0.393 | 10.232 | 9.304 | 9.117 | 4020 | 0.90 | −1.09 | 1.75 | −114.2 |
| 17303589−1638299 | 0.392 | 10.631 | 9.804 | 9.603 | 4210 | 1.25 | −0.97 | 1.55 | −104.1 |
| 17290513−1630383 | 0.380 | 10.960 | 10.090 | 9.880 | 4080 | 1.10 | −0.96 | 2.15 | −63.9 |
| 17314699−1654460 | 0.342 | 11.270 | 10.457 | 10.273 | 4215 | 1.35 | −0.93 | 1.60 | −93.5 |
| 17305076−1615216 | 0.378 | 11.238 | 10.420 | 10.218 | 4210 | 1.30 | −0.81 | 1.70 | −196.1 |
| 17323324−1627474 | 0.438 | 10.835 | 9.934 | 9.687 | 4005 | 1.05 | −0.80 | 1.75 | +40.6 |
| 17312795−1631423 | 0.412 | 11.292 | 10.466 | 10.270 | 4250 | 1.45 | −0.78 | 1.75 | +70.9 |
| 17290285−1638344 | 0.383 | 11.365 | 10.605 | 10.362 | 4255 | 1.50 | −0.73 | 2.00 | −158.2 |
| 17303378−1703086 | 0.364 | 11.011 | 10.118 | 9.906 | 4010 | 1.05 | −0.71 | 1.70 | +4.6 |
| 17304223−1609274 | 0.378 | 11.242 | 10.382 | 10.177 | 4110 | 1.35 | −0.64 | 1.65 | +78.8 |
| 17304908−1633101 | 0.400 | 10.667 | 9.831 | 9.605 | 4140 | 1.35 | −0.64 | 1.95 | −25.7 |
| 17291459−1650085 | 0.394 | 10.864 | 9.974 | 9.778 | 4080 | 1.30 | −0.62 | 1.80 | +98.1 |
| 17300674−1638541 | 0.382 | 10.903 | 10.035 | 9.823 | 4080 | 1.30 | −0.57 | 1.65 | −40.1 |
| 17315010−1653413 | 0.336 | 11.523 | 10.706 | 10.542 | 4245 | 1.60 | −0.55 | 1.75 | +37.4 |
| 17295493−1613273 | 0.375 | 11.251 | 10.391 | 10.179 | 4090 | 1.25 | −0.54 | 1.50 | −66.8 |
| 17311523−1618542 | 0.396 | 11.326 | 10.540 | 10.312 | 4245 | 1.60 | −0.52 | 1.50 | +183.9 |
| 17314811−1621558 | 0.425 | 10.998 | 10.134 | 9.927 | 4150 | 1.45 | −0.52 | 1.85 | −39.0 |
| 17304861−1646459 | 0.350 | 11.023 | 10.154 | 9.927 | 4010 | 1.25 | −0.51 | 1.60 | +73.5 |
| 17323959−1625298 | 0.439 | 11.178 | 10.363 | 10.114 | 4185 | 1.55 | −0.50 | 1.65 | −24.6 |
| 17285711−1633566 | 0.385 | 10.951 | 10.171 | 9.901 | 4150 | 1.45 | −0.50 | 1.55 | +24.5 |
| 17314673−1641228 | 0.382 | 10.655 | 9.813 | 9.553 | 4035 | 1.25 | −0.48 | 1.90 | +57.1 |
| 17294476−1626118 | 0.357 | 10.946 | 10.064 | 9.846 | 4010 | 1.30 | −0.44 | 2.10 | −139.1 |
| 17320650−1643389 | 0.394 | 10.740 | 9.880 | 9.620 | 4010 | 1.15 | −0.39 | 1.65 | +52.8 |
| 17314427−1640265 | 0.381 | 11.119 | 10.307 | 10.101 | 4215 | 1.65 | −0.39 | 1.75 | −96.9 |
| 17300064−1701075 | 0.360 | 11.003 | 10.168 | 9.900 | 4005 | 1.25 | −0.38 | 1.50 | −28.0 |
| 17302935−1652277 | 0.361 | 11.246 | 10.494 | 10.245 | 4230 | 1.60 | −0.34 | 1.70 | +17.7 |
| 17320652−1619563 | 0.421 | 11.036 | 10.162 | 9.950 | 4115 | 1.50 | −0.30 | 1.35 | +49.9 |
| 17304464−1631471 | 0.400 | 11.327 | 10.510 | 10.266 | 4145 | 1.60 | −0.29 | 1.70 | +76.1 |
| 17321715−1632467 | 0.399 | 10.671 | 9.835 | 9.616 | 4155 | 1.55 | −0.28 | 1.70 | −27.2 |
| 17321969−1653156 | 0.369 | 10.701 | 9.848 | 9.632 | 4090 | 1.45 | −0.25 | 1.40 | +100.2 |
| 17315690−1630315 | 0.412 | 11.076 | 10.212 | 9.989 | 4100 | 1.55 | −0.20 | 1.60 | +35.8 |
| 17312870−1619572 | 0.412 | 10.910 | 10.075 | 9.779 | 4010 | 1.40 | −0.19 | 1.55 | +17.7 |
| 17294541−1649018 | 0.422 | 10.704 | 9.821 | 9.582 | 4045 | 1.40 | −0.19 | 1.50 | −73.8 |
| 17305067−1644006 | 0.367 | 11.261 | 10.377 | 10.165 | 4030 | 1.45 | −0.19 | 1.65 | +21.8 |
| 17312457−1652524 | 0.327 | 11.331 | 10.548 | 10.324 | 4175 | 1.65 | −0.18 | 1.55 | +17.4 |
| 17292760−1636235 | 0.368 | 11.239 | 10.401 | 10.178 | 4105 | 1.60 | −0.18 | 1.40 | +95.9 |
| 17295978−1633590 | 0.361 | 11.161 | 10.316 | 10.077 | 4050 | 1.50 | −0.17 | 1.55 | −76.3 |
| 17322323−1649335 | 0.401 | 11.385 | 10.553 | 10.343 | 4185 | 1.65 | −0.15 | 1.75 | +65.1 |
| 17321117−1654590 | 0.356 | 10.419 | 9.638 | 9.396 | 4175 | 1.65 | −0.13 | 1.65 | −5.7 |
| 17313606−1607539 | 0.384 | 11.481 | 10.727 | 10.466 | 4230 | 1.65 | −0.11 | 1.75 | +142.4 |
| 17295331−1653069 | 0.405 | 10.744 | 9.925 | 9.695 | 4175 | 1.65 | −0.10 | 1.35 | −125.7 |
| 17302818−1636032 | 0.388 | 10.680 | 9.901 | 9.638 | 4170 | 1.60 | −0.07 | 1.40 | +42.3 |
| 17293118−1638081 | 0.371 | 10.679 | 9.901 | 9.654 | 4190 | 1.70 | −0.07 | 2.00 | −29.2 |
| 17291994−1618302 | 0.391 | 10.640 | 9.807 | 9.526 | 4020 | 1.45 | −0.07 | 1.95 | +61.4 |
| 17320457−1646391 | 0.392 | 11.037 | 10.217 | 9.960 | 4100 | 1.60 | −0.05 | 1.70 | +42.3 |
| 17310747−1620049 | 0.401 | 11.032 | 10.233 | 9.989 | 4185 | 1.65 | −0.04 | 1.50 | +80.7 |
| 17323392−1636330 | 0.403 | 11.056 | 10.172 | 9.942 | 4035 | 1.55 | −0.04 | 1.30 | +133.3 |
| 17312572−1609092 | 0.388 | 10.768 | 10.001 | 9.755 | 4240 | 1.65 | −0.03 | 1.65 | +14.6 |
| 17300015−1609464 | 0.386 | 11.432 | 10.622 | 10.405 | 4205 | 1.65 | +0.03 | 1.60 | −53.4 |
| 17305894−1637056 | 0.395 | 10.582 | 9.716 | 9.467 | 4020 | 1.50 | +0.10 | 1.30 | −46.7 |
| 17291621−1647189 | 0.412 | 10.739 | 9.855 | 9.611 | 4015 | 1.50 | +0.12 | 1.25 | −52.3 |
| 17302194−1643531 | 0.388 | 10.522 | 9.638 | 9.427 | 4055 | 1.55 | +0.14 | 1.30 | +43.6 |
| 17311959−1643577 | 0.349 | 10.989 | 10.203 | 9.947 | 4125 | 1.65 | +0.16 | 1.60 | −25.5 |
| 17311229−1659047 | 0.350 | 11.011 | 10.168 | 9.919 | 4020 | 1.55 | +0.20 | 1.20 | −90.2 |
| 17313313−1659216 | 0.355 | 10.843 | 10.098 | 9.830 | 4195 | 1.80 | +0.21 | 1.50 | +45.0 |
| 17301749−1629529 | 0.376 | 10.588 | 9.819 | 9.543 | 4150 | 1.70 | +0.23 | 1.50 | +68.8 |
| 17294261−1622440 | 0.353 | 11.368 | 10.533 | 10.316 | 4105 | 1.65 | +0.23 | 1.25 | −101.0 |
| 17323625−1637551 | 0.402 | 10.360 | 9.557 | 9.336 | 4230 | 1.80 | +0.26 | 1.45 | +53.2 |
| 17314292−1620036 | 0.419 | 10.933 | 10.095 | 9.817 | 4050 | 1.60 | +0.28 | 1.60 | −37.6 |
| 17310955−1635152 | 0.397 | 10.717 | 9.870 | 9.612 | 4045 | 1.55 | +0.32 | 1.40 | +37.0 |
| 17304312−1630318 | 0.396 | 11.403 | 10.624 | 10.369 | 4200 | 1.75 | +0.37 | 1.55 | −31.3 |
| 17285469−1627232 | 0.394 | 10.854 | 10.085 | 9.844 | 4255 | 1.90 | +0.42 | 1.35 | +15.8 |
| 17310360−1700146 | 0.355 | 10.861 | 10.086 | 9.798 | 4085 | 1.70 | +0.43 | 1.50 | −36.5 |
| 17295898−1652101 | 0.396 | 11.252 | 10.477 | 10.214 | 4190 | 1.80 | +0.59 | 1.50 | +73.1 |
3.2. Equivalent Width Abundance Determinations
The Fe i abundances were determined by measuring equivalent widths (EWs), using software developed for Johnson et al. (2008). The final [Fe/H] abundances, listed in Tables 2 and 3, were derived using the 2010 version of the LTE line analysis code MOOG (Sneden 1973). Single, isolated lines were fit with a Gaussian profile and moderately blended lines were deblended with up to five Gaussian profiles. We selected 61 Fe i lines located in the wavelength regions specified in Section 2 that were relatively isolated in the spectra of both Arcturus (Hinkle et al. 2000)17 and μ Leo (Moultaka et al. 2004).18 On average, the [Fe/H] abundances for the (−5.5, −7), (−4, −9), and (+8.5, +9) fields are based on 21 Fe i lines. The number of lines used for each star is less than the 61 potential lines due to variations in wavelength coverage (Blanco–Hydra versus WIYN–Hydra), temperature, metallicity, and S/N. The average line-to-line dispersion of 0.16 dex (σ = 0.03) was found to not vary significantly as a function of temperature or metallicity, and is reasonable given the relatively high metallicity and cool temperatures of our target stars coupled with the moderate spectral resolution.
Table 3. Chemical Abundance Ratios
| Star ID | [Fe/H] | [O/Fe] | [Si/Fe] | [Ca/Fe] |
|---|---|---|---|---|
| 2MASS | ||||
| (l, b) = (−5.5, −7) | ||||
| 18011989−3723462 | −1.50 | +0.67 | +0.30 | +0.26 |
| 18003452−3729217 | −1.40 | ... | +0.36 | +0.30 |
| 18011692−3722508 | −1.33 | +0.58 | +0.28 | +0.42 |
| 18005584−3739103 | −1.31 | +0.81 | ... | ... |
| 18015010−3735279 | −1.15 | +0.94 | +0.41 | +0.38 |
| 18005916−3727585 | −1.04 | +0.79 | +0.39 | +0.46 |
| 18005234−3715478 | −0.99 | +0.59 | +0.24 | +0.41 |
| 18005027−3707505 | −0.99 | +0.81 | +0.31 | +0.12 |
| 18020106−3737561 | −0.98 | +0.62 | +0.30 | +0.49 |
| 17595541−3713447 | −0.90 | +0.72 | ... | ... |
| 17595664−3725304 | −0.89 | +0.61 | +0.33 | +0.24 |
| 18021345−3730371 | −0.80 | ... | +0.38 | +0.43 |
| 17594241−3718247 | −0.76 | +0.61 | +0.41 | ... |
| 18013342−3726339 | −0.76 | ... | +0.31 | +0.26 |
| 18013580−3740055 | −0.75 | +0.51 | +0.43 | +0.40 |
| 18003204−3726008 | −0.75 | +0.88 | +0.35 | +0.44 |
| 18013799−3725131 | −0.74 | +0.80 | +0.45 | +0.37 |
| 18022149−3713494 | −0.71 | ... | +0.27 | +0.09 |
| 18011408−3711299 | −0.69 | +0.69 | +0.40 | +0.21 |
| 18021275−3737543 | −0.67 | ... | ... | +0.43 |
| 17595027−3727293 | −0.66 | ... | +0.21 | +0.30 |
| 18002115−3715519 | −0.61 | +0.63 | +0.27 | +0.30 |
| 17595366−3728186 | −0.59 | ... | +0.31 | +0.27 |
| 18013960−3723398 | −0.58 | +0.38 | +0.31 | +0.34 |
| 18001354−3709122 | −0.58 | +0.53 | +0.38 | +0.40 |
| 18000535−3735315 | −0.57 | +0.40 | +0.29 | +0.25 |
| 18021862−3734204 | −0.57 | ... | ... | +0.17 |
| 18013848−3721442 | −0.55 | +0.60 | +0.30 | +0.30 |
| 18014343−3708232 | −0.54 | +0.31 | +0.19 | +0.22 |
| 18004824−3718074 | −0.54 | +0.34 | +0.24 | +0.26 |
| 17594792−3721422 | −0.54 | ... | +0.25 | +0.21 |
| 18011941−3721250 | −0.54 | ... | ... | +0.27 |
| 18005852−3711524 | −0.53 | +0.56 | +0.45 | +0.59 |
| 18020816−3714015 | −0.53 | +0.58 | +0.29 | +0.28 |
| 18010932−3702079 | −0.49 | +0.39 | +0.10 | +0.19 |
| 18010065−3740456 | −0.49 | +0.74 | +0.41 | +0.29 |
| 17595640−3710383 | −0.43 | +0.31 | +0.26 | +0.38 |
| 18012462−3738382 | −0.43 | +0.63 | +0.26 | +0.32 |
| 18024484−3714159 | −0.42 | +0.27 | +0.08 | +0.28 |
| 18002880−3710171 | −0.42 | +0.32 | +0.27 | +0.34 |
| 18013206−3708133 | −0.41 | ... | ... | ... |
| 18004074−3740058 | −0.36 | +0.13 | +0.08 | +0.34 |
| 18015431−3717070 | −0.34 | +0.37 | +0.17 | +0.16 |
| 18000013−3715053 | −0.34 | +0.44 | +0.19 | +0.17 |
| 18021006−3738193 | −0.32 | +0.39 | +0.03 | +0.42 |
| 17595442−3721118 | −0.29 | +0.29 | +0.25 | +0.19 |
| 18021721−3736096 | −0.25 | +0.22 | −0.08 | +0.11 |
| 18005096−3733499 | −0.25 | +0.70 | +0.38 | ... |
| 18013395−3705551 | −0.24 | +0.29 | +0.29 | +0.36 |
| 18011851−3706092 | −0.24 | +0.34 | +0.24 | +0.29 |
| 18005923−3707111 | −0.24 | ... | +0.19 | +0.05 |
| 18022648−3728188 | −0.20 | +0.15 | +0.04 | +0.09 |
| 18024919−3727234 | −0.16 | +0.21 | +0.07 | +0.12 |
| 18023660−3716289 | −0.14 | +0.29 | +0.27 | −0.04 |
| 18005395−3731231 | −0.13 | −0.27 | +0.04 | +0.16 |
| 17595509−3711099 | −0.13 | ... | −0.20 | +0.13 |
| 18010322−3705447 | −0.10 | +0.00 | +0.04 | +0.03 |
| 18014769−3739220 | −0.10 | +0.10 | ... | ... |
| 17594807−3715283 | −0.09 | +0.14 | −0.11 | +0.32 |
| 18013618−3706311 | −0.07 | +0.25 | +0.16 | +0.01 |
| 18003751−3728200 | −0.03 | +0.03 | −0.01 | +0.09 |
| 18004314−3730156 | −0.03 | ... | −0.06 | −0.01 |
| 18014303−3740054 | −0.03 | ... | +0.03 | +0.08 |
| 18011170−3727118 | −0.01 | ... | −0.19 | −0.32 |
| 18023846−3718345 | −0.01 | ... | −0.24 | +0.21 |
| 18011671−3722213 | +0.00 | +0.10 | −0.09 | ... |
| 18005985−3734507 | +0.02 | ... | ... | ... |
| 18000430−3711051 | +0.06 | +0.38 | +0.13 | +0.14 |
| 18003552−3729476 | +0.06 | ... | −0.04 | +0.00 |
| 18001817−3732243 | +0.08 | ... | −0.08 | +0.33 |
| 18013039−3713086 | +0.09 | −0.09 | −0.03 | −0.21 |
| 18012564−3741052 | +0.10 | +0.10 | −0.16 | +0.09 |
| 18025713−3718318 | +0.10 | ... | −0.16 | +0.12 |
| 18011599−3741385 | +0.11 | +0.14 | +0.23 | −0.02 |
| 18012944−3719488 | +0.12 | ... | −0.12 | −0.03 |
| 18020361−3719086 | +0.15 | −0.20 | +0.13 | +0.00 |
| 18000412−3717266 | +0.17 | −0.32 | −0.16 | +0.14 |
| 18024024−3728187 | +0.17 | −0.12 | −0.06 | −0.20 |
| 18011177−3703344 | +0.19 | −0.09 | −0.33 | +0.09 |
| 18001410−3725181 | +0.19 | −0.09 | −0.23 | +0.11 |
| 18020300−3719418 | +0.21 | −0.09 | −0.20 | +0.06 |
| 18004683−3703252 | +0.22 | +0.08 | −0.17 | +0.15 |
| 18015404−3722564 | +0.22 | +0.38 | −0.20 | +0.04 |
| 18013974−3704068 | +0.27 | −0.05 | −0.25 | −0.02 |
| 18020704−3708064 | +0.27 | −0.02 | −0.24 | −0.02 |
| 18023393−3730273 | +0.33 | ... | ... | ... |
| 18001720−3708374 | +0.42 | −0.32 | −0.52 | −0.14 |
| 18003663−3708547 | +0.42 | ... | −0.32 | +0.01 |
| 18002569−3729578 | +0.50 | −0.25 | −0.57 | −0.03 |
| 17594881−3716203 | +0.59 | +0.01 | −0.37 | +0.01 |
| 18011201−3740090 | +0.66 | −0.26 | −0.41 | −0.23 |
| (l, b) = (−4, −9) | ||||
| 18122552−3653049 | −1.40 | +0.74 | +0.15 | +0.35 |
| 18120653−3654264 | −1.38 | ... | +0.28 | +0.40 |
| 18110179−3630394 | −1.38 | +0.53 | +0.28 | +0.43 |
| 18124892−3626403 | −1.33 | +0.71 | +0.28 | +0.43 |
| 18135164−3643463 | −1.30 | +0.70 | +0.38 | +0.34 |
| 18124339−3635339 | −1.28 | +0.75 | +0.33 | +0.44 |
| 18113921−3652069 | −1.26 | ... | +0.56 | +0.22 |
| 18111325−3646007 | −1.21 | +0.61 | +0.36 | +0.51 |
| 18113833−3626322 | −1.18 | +0.83 | +0.57 | +0.47 |
| 18111018−3639350 | −1.16 | +0.48 | +0.29 | +0.33 |
| 18135243−3630481 | −1.15 | +0.50 | +0.42 | +0.22 |
| 18121150−3627559 | −1.10 | +0.65 | +0.29 | +0.22 |
| 18111963−3647245 | −1.06 | +0.44 | +0.38 | +0.54 |
| 18140023−3635461 | −1.05 | +0.70 | +0.82 | +0.22 |
| 18135881−3639345 | −0.99 | +0.54 | +0.31 | +0.35 |
| 18121436−3654551 | −0.93 | +0.71 | +0.76 | +0.40 |
| 18124228−3655079 | −0.92 | +0.74 | +0.62 | +0.33 |
| 18122530−3637366 | −0.89 | +0.56 | +0.54 | +0.29 |
| 18131370−3651584 | −0.88 | ... | +0.53 | +0.32 |
| 18134668−3623541 | −0.88 | ... | ... | +0.28 |
| 18105081−3642137 | −0.87 | +0.57 | +0.32 | +0.57 |
| 18124219−3631172 | −0.87 | +0.57 | +0.52 | +0.41 |
| 18133688−3647054 | −0.86 | ... | ... | ... |
| 18123142−3639294 | −0.80 | +0.75 | +0.50 | +0.47 |
| 18133038−3632229 | −0.80 | ... | +0.25 | ... |
| 18133292−3624179 | −0.78 | +0.58 | ... | ... |
| 18111681−3636318 | −0.77 | +0.53 | +0.34 | +0.25 |
| 18105004−3640063 | −0.76 | +0.46 | +0.26 | ... |
| 18112334−3634194 | −0.74 | +0.49 | +0.36 | +0.51 |
| 18131027−3632343 | −0.73 | +0.54 | +0.39 | +0.38 |
| 18110293−3628041 | −0.72 | +0.65 | +0.71 | +0.32 |
| 18132040−3623075 | −0.71 | +0.74 | +0.38 | +0.43 |
| 18135588−3629188 | −0.71 | +0.88 | +0.29 | +0.20 |
| 18105075−3635061 | −0.70 | +0.55 | +0.38 | +0.33 |
| 18104188−3634541 | −0.68 | +0.73 | +0.28 | +0.14 |
| 18132998−3628578 | −0.68 | +0.72 | +0.33 | +0.19 |
| 18130544−3616563 | −0.66 | ... | +0.50 | +0.48 |
| 18115908−3654510 | −0.64 | +0.49 | +0.48 | +0.30 |
| 18121077−3639094 | −0.63 | +0.53 | +0.38 | +0.11 |
| 18120614−3629571 | −0.58 | +0.23 | +0.38 | +0.18 |
| 18120213−3641599 | −0.55 | ... | +0.47 | +0.26 |
| 18123350−3654398 | −0.54 | ... | +0.70 | +0.42 |
| 18120973−3654184 | −0.53 | +0.78 | +0.78 | +0.17 |
| 18105641−3632359 | −0.52 | +0.32 | +0.52 | +0.38 |
| 18125106−3654091 | −0.51 | +0.26 | +0.21 | +0.21 |
| 18111581−3648469 | −0.51 | +0.28 | +0.40 | +0.36 |
| 18131387−3630130 | −0.51 | ... | +0.25 | +0.24 |
| 18123592−3634476 | −0.50 | +0.52 | +0.28 | +0.17 |
| 18135736−3638266 | −0.49 | +0.24 | +0.24 | +0.39 |
| 18133233−3626133 | −0.49 | +0.48 | +0.21 | +0.19 |
| 18125003−3630269 | −0.49 | +0.29 | +0.49 | +0.16 |
| 18130723−3618385 | −0.45 | +0.55 | +0.42 | +0.40 |
| 18125800−3616427 | −0.44 | +0.34 | +0.13 | +0.45 |
| 18111323−3637030 | −0.44 | +0.04 | +0.13 | +0.29 |
| 18130427−3630012 | −0.44 | +0.09 | +0.34 | +0.14 |
| 18124614−3617326 | −0.43 | ... | +0.45 | +0.07 |
| 18120399−3615387 | −0.43 | +0.28 | +0.12 | +0.21 |
| 18123475−3624478 | −0.43 | +0.53 | +0.33 | +0.31 |
| 18115661−3617533 | −0.41 | +0.11 | +0.32 | +0.55 |
| 18113299−3623341 | −0.40 | +0.31 | +0.32 | +0.41 |
| 18111553−3628156 | −0.37 | +0.62 | +0.35 | +0.31 |
| 18125907−3644275 | −0.37 | +0.07 | +0.25 | +0.03 |
| 18111726−3620302 | −0.34 | +0.26 | ... | +0.22 |
| 18111579−3625114 | −0.34 | +0.43 | +0.29 | +0.54 |
| 18131305−3650449 | −0.33 | ... | +0.34 | +0.25 |
| 18123152−3636498 | −0.33 | +0.28 | +0.35 | +0.37 |
| 18125914−3619208 | −0.30 | +0.27 | +0.21 | +0.30 |
| 18115073−3650493 | −0.29 | ... | +0.33 | +0.20 |
| 18114648−3625169 | −0.28 | ... | +0.41 | +0.18 |
| 18113751−3629139 | −0.28 | ... | +0.41 | +0.38 |
| 18122243−3637539 | −0.24 | +0.30 | +0.13 | +0.30 |
| 18133366−3644575 | −0.23 | +0.25 | +0.28 | ... |
| 18134702−3641477 | −0.23 | +0.33 | +0.41 | +0.28 |
| 18125228−3618294 | −0.21 | −0.14 | +0.11 | +0.31 |
| 18110942−3647198 | −0.21 | ... | +0.06 | −0.08 |
| 18104824−3638507 | −0.19 | +0.09 | +0.09 | +0.22 |
| 18122301−3629462 | −0.19 | +0.13 | +0.11 | +0.14 |
| 18133332−3645578 | −0.18 | +0.28 | +0.30 | +0.23 |
| 18123434−3652241 | −0.18 | +0.39 | +0.24 | +0.10 |
| 18112311−3625456 | −0.17 | −0.01 | +0.12 | +0.26 |
| 18125463−3649277 | −0.14 | +0.54 | +0.20 | +0.16 |
| 18123925−3620465 | −0.14 | ... | +0.02 | +0.18 |
| 18110629−3632146 | −0.13 | −0.07 | +0.05 | +0.07 |
| 18133687−3639590 | −0.11 | +0.21 | +0.19 | +0.39 |
| 18111505−3620576 | −0.09 | −0.06 | +0.01 | +0.33 |
| 18120832−3628243 | −0.09 | +0.15 | +0.24 | +0.28 |
| 18130815−3631460 | −0.09 | +0.14 | +0.17 | +0.27 |
| 18120407−3636481 | −0.09 | +0.29 | +0.06 | +0.14 |
| 18135786−3640300 | −0.05 | −0.10 | −0.05 | +0.12 |
| 18131228−3619138 | −0.04 | −0.21 | +0.05 | +0.22 |
| 18113372−3650200 | −0.04 | −0.11 | ... | +0.03 |
| 18115904−3650428 | −0.01 | ... | +0.06 | +0.00 |
| 18115448−3641161 | −0.01 | +0.05 | +0.04 | −0.04 |
| 18123678−3649019 | +0.02 | +0.33 | −0.12 | +0.20 |
| 18113965−3645408 | +0.05 | ... | −0.40 | −0.07 |
| 18135362−3636538 | +0.06 | ... | −0.04 | +0.31 |
| 18123168−3631555 | +0.09 | +0.01 | −0.24 | +0.09 |
| 18115398−3623290 | +0.09 | +0.51 | −0.09 | +0.14 |
| 18123393−3615508 | +0.11 | ... | +0.00 | +0.16 |
| 18120689−3643231 | +0.11 | −0.31 | −0.01 | −0.07 |
| 18130482−3649019 | +0.13 | +0.11 | −0.13 | ... |
| 18110352−3646275 | +0.14 | +0.01 | −0.07 | −0.05 |
| 18105013−3629557 | +0.17 | −0.22 | −0.12 | +0.21 |
| 18121897−3630243 | +0.22 | ... | +0.08 | +0.14 |
| 18122029−3652333 | +0.26 | ... | −0.09 | +0.12 |
| (l, b) = (+8.5, +9) | ||||
| 17311256−1702018 | −1.26 | +0.76 | +0.31 | +0.34 |
| 17290874−1632431 | −1.23 | +0.70 | +0.31 | +0.30 |
| 17302885−1639588 | −1.17 | +0.57 | +0.46 | +0.36 |
| 17304789−1623192 | −1.14 | +0.64 | +0.36 | +0.44 |
| 17321080−1641479 | −1.09 | +0.77 | +0.27 | +0.27 |
| 17303589−1638299 | −0.97 | +0.66 | +0.42 | +0.44 |
| 17290513−1630383 | −0.96 | +0.84 | +0.57 | +0.40 |
| 17314699−1654460 | −0.93 | +0.73 | +0.24 | +0.33 |
| 17305076−1615216 | −0.81 | +0.66 | +0.46 | +0.37 |
| 17323324−1627474 | −0.80 | +0.38 | +0.54 | ... |
| 17312795−1631423 | −0.78 | +0.56 | +0.33 | +0.15 |
| 17290285−1638344 | −0.73 | +0.60 | +0.37 | +0.21 |
| 17303378−1703086 | −0.71 | +0.51 | +0.38 | +0.27 |
| 17304223−1609274 | −0.64 | +0.59 | +0.39 | +0.15 |
| 17304908−1633101 | −0.64 | ... | +0.31 | +0.14 |
| 17291459−1650085 | −0.62 | +0.55 | +0.27 | +0.00 |
| 17300674−1638541 | −0.57 | ... | +0.40 | +0.31 |
| 17315010−1653413 | −0.55 | +0.59 | +0.46 | +0.37 |
| 17295493−1613273 | −0.54 | ... | +0.54 | +0.22 |
| 17311523−1618542 | −0.52 | ... | +0.46 | ... |
| 17314811−1621558 | −0.52 | +0.21 | +0.33 | +0.00 |
| 17304861−1646459 | −0.51 | +0.56 | +0.31 | +0.11 |
| 17323959−1625298 | −0.50 | ... | +0.43 | +0.22 |
| 17285711−1633566 | −0.50 | +0.50 | +0.33 | +0.16 |
| 17314673−1641228 | −0.48 | +0.46 | +0.28 | +0.35 |
| 17294476−1626118 | −0.44 | +0.39 | +0.25 | +0.27 |
| 17320650−1643389 | −0.39 | +0.19 | +0.11 | +0.09 |
| 17314427−1640265 | −0.39 | +0.46 | +0.30 | +0.19 |
| 17300064−1701075 | −0.38 | ... | +0.08 | −0.01 |
| 17302935−1652277 | −0.34 | −0.31 | +0.12 | −0.11 |
| 17320652−1619563 | −0.30 | +0.27 | +0.33 | +0.45 |
| 17304464−1631471 | −0.29 | +0.69 | +0.25 | +0.24 |
| 17321715−1632467 | −0.28 | ... | +0.30 | −0.04 |
| 17321969−1653156 | −0.25 | +0.55 | +0.13 | +0.14 |
| 17315690−1630315 | −0.20 | +0.22 | +0.35 | +0.18 |
| 17312870−1619572 | −0.19 | +0.30 | +0.14 | +0.03 |
| 17294541−1649018 | −0.19 | +0.29 | +0.01 | +0.07 |
| 17305067−1644006 | −0.19 | +0.23 | +0.00 | −0.10 |
| 17312457−1652524 | −0.18 | +0.48 | +0.29 | +0.20 |
| 17292760−1636235 | −0.18 | +0.68 | −0.03 | +0.12 |
| 17295978−1633590 | −0.17 | ... | +0.04 | −0.09 |
| 17322323−1649335 | −0.15 | +0.32 | +0.20 | +0.02 |
| 17321117−1654590 | −0.13 | +0.08 | +0.12 | +0.25 |
| 17313606−1607539 | −0.11 | +0.41 | +0.27 | −0.07 |
| 17295331−1653069 | −0.10 | +0.52 | +0.20 | +0.20 |
| 17302818−1636032 | −0.07 | +0.32 | +0.05 | +0.10 |
| 17293118−1638081 | −0.07 | ... | −0.01 | +0.00 |
| 17291994−1618302 | −0.07 | +0.29 | +0.01 | −0.29 |
| 17320457−1646391 | −0.05 | +0.17 | +0.02 | +0.08 |
| 17310747−1620049 | −0.04 | +0.44 | +0.09 | +0.26 |
| 17323392−1636330 | −0.04 | −0.05 | ... | +0.11 |
| 17312572−1609092 | −0.03 | −0.04 | +0.09 | +0.19 |
| 17300015−1609464 | +0.03 | ... | −0.13 | +0.11 |
| 17305894−1637056 | +0.10 | +0.29 | −0.30 | −0.09 |
| 17291621−1647189 | +0.12 | +0.18 | −0.12 | −0.27 |
| 17302194−1643531 | +0.14 | +0.26 | −0.29 | −0.12 |
| 17311959−1643577 | +0.16 | ... | −0.23 | −0.06 |
| 17311229−1659047 | +0.20 | ... | −0.30 | −0.13 |
| 17313313−1659216 | +0.21 | +0.17 | −0.18 | −0.04 |
| 17301749−1629529 | +0.23 | −0.08 | −0.26 | −0.07 |
| 17294261−1622440 | +0.23 | ... | −0.38 | −0.23 |
| 17323625−1637551 | +0.26 | −0.33 | −0.28 | +0.07 |
| 17314292−1620036 | +0.28 | ... | −0.32 | −0.22 |
| 17310955−1635152 | +0.32 | −0.27 | −0.12 | −0.11 |
| 17304312−1630318 | +0.37 | ... | −0.32 | +0.09 |
| 17285469−1627232 | +0.42 | +0.05 | −0.30 | −0.03 |
| 17310360−1700146 | +0.43 | ... | −0.18 | +0.07 |
| 17295898−1652101 | +0.59 | −0.17 | −0.44 | −0.11 |
The Fe i abundances were determined on a line-by-line basis relative to Arcturus. The oscillator strength (log gf) values listed in Table 4 were derived by measuring the EW of each line in the high resolution, high S/N Arcturus atlas and forcing the derived abundance for each line to be [Fe/H] = −0.50, assuming the Arcturus model atmosphere parameters given in Fulbright et al. (2006; Teff = 4290 K, log(g) = 1.60, [Fe/H] = −0.50, and vt = 1.67 km s-1). The wavelength and excitation potential values given in Table 4 are from the NIST Atomic Spectra Database (Ralchenko et al. 2011),19 Vienna Atomic Line Database (VALD; Kupka et al. 2000),20 or Thevenin (1990). Sample spectra of both the 6250 and 6700 Å setups for stars with similar Teff but different [Fe/H] are shown in Figure 3. This figure also illustrates data quality as well as the change in line strength, continuum availability, and molecular contamination as a function of [Fe/H].
Figure 3. Typical sample spectra for stars of comparable Teff are shown to illustrate how the continuum windows, line strengths, and molecular features change as a function of metallicity. The left panel shows a portion of the 6300 Å region spectra, and the right panel shows a portion of the 6700 Å region spectra for the same three stars. The spectra have been offset for display purposes.
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Standard image High-resolution imageTable 4. Line List
| Element | Wavelength | E.P. | log gf | Arcturus [Fe/H] or [X/Fe] |
|---|---|---|---|---|
| (Å) | (eV) | |||
| Fe i | 6056.00 | 4.73 | −0.40 | −0.50 |
| Fe i | 6062.85 | 2.18 | −4.00 | −0.50 |
| Fe i | 6065.48 | 2.61 | −1.56 | −0.50 |
| Fe i | 6078.49 | 4.80 | −0.46 | −0.50 |
| Fe i | 6079.01 | 4.65 | −1.13 | −0.50 |
| Fe i | 6093.64 | 4.61 | −1.47 | −0.50 |
| Fe i | 6094.37 | 4.65 | −1.70 | −0.50 |
| Fe i | 6096.66 | 3.98 | −1.96 | −0.50 |
| Fe i | 6098.24 | 4.56 | −1.80 | −0.50 |
| Fe i | 6102.17 | 4.83 | −0.30 | −0.50 |
| Fe i | 6105.13 | 4.55 | −1.97 | −0.50 |
| Fe i | 6120.25 | 0.92 | −5.94 | −0.50 |
| Fe i | 6127.91 | 4.14 | −1.49 | −0.50 |
| Fe i | 6151.62 | 2.18 | −3.27 | −0.50 |
| Fe i | 6156.81 | 4.96 | −2.24 | −0.50 |
| Fe i | 6165.36 | 4.14 | −1.64 | −0.50 |
| Fe i | 6173.34 | 2.22 | −2.87 | −0.50 |
| Fe i | 6187.40 | 2.83 | −4.14 | −0.50 |
| Fe i | 6187.99 | 3.94 | −1.62 | −0.50 |
| Fe i | 6200.31 | 2.61 | −2.33 | −0.50 |
| Fe i | 6207.23 | 4.99 | −1.80 | −0.50 |
| Fe i | 6226.74 | 3.88 | −2.10 | −0.50 |
| Fe i | 6232.64 | 3.65 | −1.11 | −0.50 |
| Fe i | 6240.65 | 2.22 | −3.34 | −0.50 |
| Fe i | 6246.32 | 3.60 | −0.77 | −0.50 |
| Fe i | 6252.56 | 2.40 | −1.63 | −0.50 |
| Fe i | 6270.23 | 2.86 | −2.57 | −0.50 |
| Fe i | 6290.54 | 2.59 | −4.39 | −0.50 |
| Fe i | 6297.79 | 2.22 | −2.67 | −0.50 |
| Fe i | 6301.50 | 3.65 | −0.67 | −0.50 |
| Fe i | 6302.49 | 3.69 | −1.12 | −0.50 |
| Fe i | 6307.85 | 3.64 | −3.27 | −0.50 |
| Fe i | 6315.81 | 4.08 | −1.57 | −0.50 |
| Fe i | 6322.69 | 2.59 | −2.26 | −0.50 |
| Fe i | 6330.85 | 4.73 | −1.16 | −0.50 |
| Fe i | 6574.25 | 0.99 | −4.76 | −0.50 |
| Fe i | 6591.33 | 4.59 | −1.96 | −0.50 |
| Fe i | 6593.88 | 2.43 | −2.15 | −0.50 |
| Fe i | 6597.56 | 4.80 | −1.03 | −0.50 |
| Fe i | 6627.56 | 4.55 | −1.40 | −0.50 |
| Fe i | 6633.75 | 4.56 | −0.89 | −0.50 |
| Fe i | 6646.97 | 2.61 | −3.80 | −0.50 |
| Fe i | 6648.12 | 1.01 | −5.67 | −0.50 |
| Fe i | 6653.91 | 4.15 | −2.25 | −0.50 |
| Fe i | 6667.42 | 2.45 | −4.43 | −0.50 |
| Fe i | 6678.00 | 2.69 | −1.17 | −0.50 |
| Fe i | 6692.27 | 4.08 | −3.15 | −0.50 |
| Fe i | 6703.58 | 2.76 | −2.88 | −0.50 |
| Fe i | 6704.48 | 4.22 | −2.60 | −0.50 |
| Fe i | 6710.32 | 1.48 | −4.80 | −0.50 |
| Fe i | 6713.74 | 4.80 | −1.53 | −0.50 |
| Fe i | 6725.36 | 4.10 | −2.20 | −0.50 |
| Fe i | 6726.67 | 4.61 | −1.07 | −0.50 |
| Fe i | 6730.29 | 4.91 | −2.24 | −0.50 |
| Fe i | 6733.15 | 4.64 | −1.58 | −0.50 |
| Fe i | 6739.52 | 1.56 | −5.03 | −0.50 |
| Fe i | 6745.96 | 4.08 | −2.85 | −0.50 |
| Fe i | 6746.95 | 2.61 | −4.43 | −0.50 |
| Fe i | 6750.16 | 2.42 | −2.57 | −0.50 |
| Fe i | 6793.27 | 4.07 | −2.33 | −0.50 |
| Fe i | 6810.26 | 4.61 | −1.10 | −0.50 |
| O i | 6300.31 | 0.00 | −10.00 | +0.48 |
| Si i | 6145.01 | 5.62 | −1.50 | +0.35 |
| Si i | 6155.13 | 5.62 | −0.97 | +0.35 |
| Ca i | 6156.01 | 2.52 | −2.61 | +0.21 |
| Ca i | 6166.44 | 2.52 | −1.24 | +0.21 |
| Ca i | 6169.04 | 2.52 | −0.90 | +0.21 |
| Ca i | 6169.56 | 2.52 | −0.67 | +0.21 |
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3.3. Spectrum Synthesis Abundance Determinations
For the elements other than Fe, we determined abundances via spectrum synthesis rather than EW measurement. Given the large number of stars analyzed here, we employed the computationally parallel version of the MOOG synth driver developed for Johnson et al. (2012). Similar to the Fe abundance measurements, [O/Fe], [Si/Fe], and [Ca/Fe] ratios were determined relative to Arcturus. We adopted the Arcturus abundances derived in Fulbright et al. (2007): [O/Fe] = +0.48, [Si/Fe] = +0.35, and [Ca/Fe] = +0.21. These adopted values are within ∼0.1 dex of those derived recently by Ramírez & Allende Prieto (2011). The lines used here are listed in Table 3.
For the 6300 Å [O i] line we synthesized the region spanning 6295–6305 Å, including the 6300.34 Å Ni i line that is blended with the 6300.30 [O i] feature. We assumed [Ni/Fe] = 0 for all syntheses. The initial line list was compiled from VALD for atomic lines and the Kurucz database21 for CN molecular lines. The final log gf values for all significant atomic and molecular lines in the 6295–6305 Å region were adjusted to minimize the difference between our synthetic spectrum and the Arcturus atlas. In order to fit the CN features, we adopted the Arcturus carbon and nitrogen abundances from Peterson et al. (1993; [C/Fe] = +0.0 and [N/Fe] = +0.3). In general this provided a satisfactory fit to the CN lines using the original Kurucz line list and only a few minor adjustments were required. For the Sc I line that is blended with the [O i] feature in our Hydra spectra but not the Arcturus atlas, we set the log gf value assuming [Sc/Fe] = +0.2 (Peterson et al. 1993). However, as can be seen in the sample syntheses provided in Figure 4, there is enough separation between the [O i] and Sc features in the Hydra spectra to reasonably account for the Sc contribution.
Figure 4. Sample spectrum synthesis fits to the region around the 6300 Å [O i] line for a cool metal-poor star (left panels) and a cool metal-rich star (right panels). In the top left and top right panels, the solid black line shows the best fit oxygen abundance. The colored solid lines illustrate how the syntheses change when the oxygen abundance is altered by +0.3 dex (red lines) and −0.3 dex (blue lines) from the best-fit value. Similarly, the bottom left and bottom right panels show how the syntheses change when oxygen is held fixed at the best-fit value while the CN and Sc abundances are altered by ±0.3 dex.
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Standard image High-resolution imageSince the [O i] line is both modestly affected by CN blending (see bottom panels of Figure 4) and also by the C+N abundance (via the molecular equilibrium calculation), we identified a small window in the 6250 Å spectra that could be used to roughly estimate the CN abundance. While there are other similar windows that may be used, especially in the 6700 Å spectra, we selected the 6331–6339 Å window (shown in Figure 5) because it provided a several Angstrom wide region comprised of mostly CN lines and was observed with both the WIYN and Blanco bench spectrographs. For each star we initially set [C/Fe] = −0.30 and [N/Fe] = +0.50, values typical for bulge RGB stars (e.g., Meléndez et al. 2008; Ryde et al. 2010), and then adjusted [N/Fe] until a satisfactory fit was found. The derived [C/Fe] and [N/Fe] abundances were then used in the [O i] synthesis. This processes was iterated at least once for each star to account for the correlated variations in line strength between CN and O.
Figure 5. Similar to Figure 4, the synthetic spectrum fits shown here illustrate how the CN abundance was determined for each star. The top panel shows a cool, metal-poor example and the bottom panel shows a cool, metal-rich example. The black line indicates the best fit CN abundance. The red and blue syntheses indicate changes in the CN abundance by ±0.3 dex, respectively. Note that except for a weak Si i and Fe ii blend near 6332 Å, the two regions spanning 6331.5–6335 Å and 6337.5–6339.8 Å contain almost exclusively CN features.
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Standard image High-resolution imageThe Si and Ca abundances are based on synthesis fits to lines in the 6140–6170 Å window. In order to properly account for CN contamination, Si and Ca were measured after obtaining CNO abundances. For the few stars where [O i] could not be measured, we have adopted the general [O/Fe] versus [Fe/H] trend found in our data (see Section 4.3). Sample Si and Ca synthesis fits for a cool, metal-rich giant are shown in Figure 6. While most of the lines are not strongly affected by CN, the 6155 Å Si i line is sensitive to the CN abundance in our most metal-rich giants. As can be seen in Figure 6, changing the CN abundance by ±0.3 dex can result in a Si abundance uncertainty ≳0.2 dex. A comparison between the 6155 Å Si abundance and the 6145 Å Si abundance, which is only weakly affected by CN, suggests that at least on average there is reasonable agreement with 〈[Si/Fe]6155–[Si/Fe]6145〉 = −0.03 (σ = 0.17). The four Ca lines used here exhibit a similar degree of agreement with an average line-to-line dispersion of 0.08 dex (σ = 0.05).
Figure 6. Similar to Figure 4, the synthetic spectrum fits shown here illustrate how the Si and Ca line profiles change when the Si and Ca abundances are altered ±0.3 dex from the best-fit value (top panel) and when the CN abundance is altered by ±0.3 dex from the best-fit value (bottom panel). Note the particular sensitivity of the 6155 Å Si i line to changes in the CN abundance.
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Standard image High-resolution image3.4. Abundance Uncertainty Estimates
Tables 5–8 summarize the abundance uncertainty estimates for log (Fe), log (O), log (Si), and log (Ca) due to changes in Teff +100 K, log(g)+0.30, [M/H]+0.30, and vt+0.30 km s-1. The σ/√(N) values for each element are also given as an estimate of the measurement uncertainty. For elements in Tables 6–8 where only one line was available for measurement (e.g., [O i]), a value of σ/√(N) = 0.05 has been assigned. This represents the average value for cases where multiple lines could be measured, and is a reasonable uncertainty estimate for visually fitting synthetic spectra. The total error column in Tables 5–8 reflects the Teff, log(g), [M/H], vt, and measurement uncertainties added in quadrature, and are reflected in the error bars of all subsequent figures.
Table 5. Abundance Uncertainty: Iron
| Star ID | ΔTeff | Δlog(g) | Δ[M/H] | ΔVt | σ/√(N) | ΔTotal |
|---|---|---|---|---|---|---|
| 2MASS | (+100 K) | (+0.3 cgs) | (+0.3 dex) | (+0.3 km s-1) | ||
| (l, b) = (−5.5, −7) | ||||||
| 18011989−3723462 | +0.10 | +0.02 | +0.01 | −0.06 | 0.03 | 0.12 |
| 18003452−3729217 | +0.10 | +0.01 | +0.00 | −0.04 | 0.03 | 0.11 |
| 18011692−3722508 | +0.10 | +0.03 | +0.02 | −0.06 | 0.04 | 0.13 |
| 18005584−3739103 | +0.08 | +0.03 | +0.03 | −0.06 | 0.03 | 0.11 |
| 18015010−3735279 | +0.08 | +0.04 | +0.03 | −0.07 | 0.03 | 0.12 |
| 18005916−3727585 | +0.08 | +0.03 | +0.03 | −0.07 | 0.03 | 0.12 |
| 18005027−3707505 | +0.08 | +0.03 | +0.02 | −0.06 | 0.04 | 0.11 |
| 18005234−3715478 | +0.07 | +0.05 | +0.04 | −0.09 | 0.03 | 0.13 |
| 18020106−3737561 | +0.07 | +0.05 | +0.04 | −0.08 | 0.04 | 0.13 |
| 17595541−3713447 | +0.07 | +0.03 | +0.03 | −0.08 | 0.04 | 0.12 |
| 17595664−3725304 | +0.07 | +0.03 | +0.03 | −0.09 | 0.03 | 0.13 |
| 18021345−3730371 | +0.03 | +0.07 | +0.05 | −0.09 | 0.04 | 0.13 |
| 17594241−3718247 | +0.05 | +0.05 | +0.04 | −0.08 | 0.04 | 0.12 |
| 18013342−3726339 | +0.06 | +0.04 | +0.04 | −0.08 | 0.03 | 0.12 |
| 18003204−3726008 | +0.02 | +0.06 | +0.06 | −0.11 | 0.03 | 0.14 |
| 18013580−3740055 | +0.02 | +0.07 | +0.06 | −0.10 | 0.04 | 0.14 |
| 18013799−3725131 | +0.02 | +0.07 | +0.06 | −0.10 | 0.03 | 0.14 |
| 18022149−3713494 | +0.03 | +0.07 | +0.06 | −0.10 | 0.03 | 0.14 |
| 18011408−3711299 | +0.06 | +0.04 | +0.04 | −0.09 | 0.03 | 0.13 |
| 18021275−3737543 | +0.06 | +0.05 | +0.04 | −0.10 | 0.04 | 0.14 |
| 17595027−3727293 | +0.02 | +0.06 | +0.06 | −0.10 | 0.05 | 0.14 |
| 18002115−3715519 | +0.01 | +0.07 | +0.08 | −0.11 | 0.03 | 0.16 |
| 17595366−3728186 | +0.06 | +0.05 | +0.05 | −0.09 | 0.04 | 0.14 |
| 18001354−3709122 | +0.01 | +0.09 | +0.08 | −0.11 | 0.03 | 0.17 |
| 18013960−3723398 | +0.01 | +0.09 | +0.08 | −0.12 | 0.03 | 0.17 |
| 18021862−3734204 | +0.01 | +0.08 | +0.08 | −0.11 | 0.05 | 0.17 |
| 18000535−3735315 | +0.01 | +0.08 | +0.08 | −0.12 | 0.03 | 0.17 |
| 18013848−3721442 | +0.02 | +0.08 | +0.08 | −0.11 | 0.04 | 0.16 |
| 17594792−3721422 | +0.04 | +0.04 | +0.06 | −0.11 | 0.03 | 0.14 |
| 18011941−3721250 | +0.01 | +0.09 | +0.08 | −0.10 | 0.04 | 0.16 |
| 18004824−3718074 | +0.00 | +0.08 | +0.09 | −0.12 | 0.04 | 0.17 |
| 18014343−3708232 | +0.01 | +0.09 | +0.08 | −0.12 | 0.03 | 0.17 |
| 18005852−3711524 | +0.06 | +0.05 | +0.04 | −0.10 | 0.03 | 0.14 |
| 18020816−3714015 | +0.05 | +0.05 | +0.05 | −0.10 | 0.04 | 0.14 |
| 18010932−3702079 | +0.00 | +0.09 | +0.09 | −0.11 | 0.04 | 0.17 |
| 18010065−3740456 | +0.00 | +0.09 | +0.09 | −0.12 | 0.04 | 0.18 |
| 17595640−3710383 | +0.03 | +0.04 | +0.06 | −0.12 | 0.02 | 0.14 |
| 18012462−3738382 | +0.05 | +0.06 | +0.05 | −0.10 | 0.04 | 0.14 |
| 18002880−3710171 | +0.06 | +0.05 | +0.04 | −0.09 | 0.03 | 0.13 |
| 18024484−3714159 | +0.06 | +0.05 | +0.04 | −0.11 | 0.03 | 0.14 |
| 18013206−3708133 | +0.06 | +0.05 | +0.04 | −0.11 | 0.05 | 0.15 |
| 18004074−3740058 | +0.03 | +0.05 | +0.05 | −0.11 | 0.03 | 0.14 |
| 18000013−3715053 | +0.02 | +0.06 | +0.06 | −0.12 | 0.03 | 0.15 |
| 18015431−3717070 | +0.04 | +0.06 | +0.05 | −0.12 | 0.05 | 0.16 |
| 18021006−3738193 | +0.06 | +0.05 | +0.04 | −0.10 | 0.03 | 0.14 |
| 17595442−3721118 | +0.01 | +0.07 | +0.05 | −0.12 | 0.03 | 0.15 |
| 18021721−3736096 | +0.05 | +0.06 | +0.04 | −0.10 | 0.05 | 0.14 |
| 18005096−3733499 | +0.01 | +0.05 | +0.06 | −0.13 | 0.03 | 0.15 |
| 18005923−3707111 | −0.01 | +0.06 | +0.06 | −0.13 | 0.04 | 0.16 |
| 18011851−3706092 | +0.00 | +0.07 | +0.06 | −0.12 | 0.03 | 0.15 |
| 18013395−3705551 | −0.01 | +0.08 | +0.06 | −0.13 | 0.03 | 0.17 |
| 18022648−3728188 | +0.04 | +0.07 | +0.05 | −0.11 | 0.02 | 0.15 |
| 18024919−3727234 | +0.05 | +0.07 | +0.05 | −0.11 | 0.05 | 0.16 |
| 18023660−3716289 | +0.04 | +0.06 | +0.05 | −0.11 | 0.03 | 0.14 |
| 17595509−3711099 | +0.02 | +0.06 | +0.06 | −0.12 | 0.03 | 0.15 |
| 18005395−3731231 | −0.01 | +0.08 | +0.06 | −0.12 | 0.04 | 0.16 |
| 18010322−3705447 | +0.05 | +0.06 | +0.05 | −0.11 | 0.03 | 0.15 |
| 18014769−3739220 | +0.05 | +0.06 | +0.05 | −0.13 | 0.04 | 0.16 |
| 17594807−3715283 | +0.04 | +0.07 | +0.06 | −0.13 | 0.04 | 0.17 |
| 18013618−3706311 | +0.00 | +0.05 | +0.07 | −0.14 | 0.04 | 0.17 |
| 18004314−3730156 | +0.03 | +0.07 | +0.07 | −0.13 | 0.05 | 0.17 |
| 18014303−3740054 | +0.01 | +0.06 | +0.07 | −0.13 | 0.03 | 0.16 |
| 18003751−3728200 | −0.02 | +0.09 | +0.08 | −0.15 | 0.03 | 0.20 |
| 18011170−3727118 | +0.06 | +0.05 | +0.05 | −0.12 | 0.04 | 0.16 |
| 18023846−3718345 | +0.01 | +0.07 | +0.08 | −0.12 | 0.04 | 0.17 |
| 18011671−3722213 | +0.05 | +0.05 | +0.06 | −0.13 | 0.04 | 0.16 |
| 18005985−3734507 | −0.01 | +0.06 | +0.09 | −0.14 | 0.03 | 0.18 |
| 18000430−3711051 | +0.00 | +0.06 | +0.08 | −0.14 | 0.02 | 0.17 |
| 18003552−3729476 | +0.01 | +0.07 | +0.08 | −0.13 | 0.04 | 0.17 |
| 18001817−3732243 | +0.03 | +0.07 | +0.07 | −0.14 | 0.03 | 0.18 |
| 18013039−3713086 | −0.01 | +0.08 | +0.08 | −0.13 | 0.04 | 0.18 |
| 18012564−3741052 | +0.01 | +0.08 | +0.08 | −0.13 | 0.05 | 0.18 |
| 18025713−3718318 | −0.01 | +0.08 | +0.08 | −0.14 | 0.05 | 0.19 |
| 18011599−3741385 | +0.00 | +0.07 | +0.08 | −0.14 | 0.04 | 0.18 |
| 18012944−3719488 | +0.05 | +0.06 | +0.06 | −0.12 | 0.03 | 0.16 |
| 18020361−3719086 | +0.02 | +0.08 | +0.07 | −0.13 | 0.04 | 0.17 |
| 18024024−3728187 | −0.02 | +0.07 | +0.08 | −0.14 | 0.06 | 0.19 |
| 18000412−3717266 | −0.02 | +0.06 | +0.08 | −0.14 | 0.04 | 0.18 |
| 18011177−3703344 | +0.00 | +0.07 | +0.08 | −0.15 | 0.03 | 0.19 |
| 18001410−3725181 | −0.03 | +0.07 | +0.08 | −0.15 | 0.03 | 0.19 |
| 18020300−3719418 | −0.02 | +0.06 | +0.07 | −0.16 | 0.04 | 0.19 |
| 18004683−3703252 | −0.03 | +0.08 | +0.07 | −0.15 | 0.06 | 0.20 |
| 18015404−3722564 | +0.00 | +0.07 | +0.06 | −0.15 | 0.04 | 0.18 |
| 18013974−3704068 | +0.00 | +0.07 | +0.08 | −0.15 | 0.03 | 0.19 |
| 18020704−3708064 | +0.03 | +0.08 | +0.06 | −0.15 | 0.04 | 0.19 |
| 18023393−3730273 | +0.03 | +0.08 | +0.06 | −0.14 | 0.06 | 0.18 |
| 18001720−3708374 | −0.03 | +0.06 | +0.09 | −0.16 | 0.03 | 0.20 |
| 18003663−3708547 | −0.01 | +0.08 | +0.08 | −0.16 | 0.04 | 0.20 |
| 18002569−3729578 | +0.02 | +0.09 | +0.07 | −0.16 | 0.03 | 0.20 |
| 17594881−3716203 | −0.01 | +0.09 | +0.08 | −0.17 | 0.04 | 0.21 |
| 18011201−3740090 | +0.02 | +0.08 | +0.07 | −0.17 | 0.05 | 0.21 |
| (l, b) = (−4, −9) | ||||||
| 18122552−3653049 | +0.10 | +0.01 | +0.00 | −0.06 | 0.05 | 0.13 |
| 18120653−3654264 | +0.10 | +0.01 | +0.00 | −0.06 | 0.02 | 0.12 |
| 18110179−3630394 | +0.10 | +0.01 | +0.01 | −0.05 | 0.04 | 0.12 |
| 18124892−3626403 | +0.09 | +0.01 | +0.01 | −0.05 | 0.04 | 0.11 |
| 18135164−3643463 | +0.10 | +0.02 | +0.02 | −0.05 | 0.05 | 0.13 |
| 18124339−3635339 | +0.10 | +0.02 | +0.02 | −0.06 | 0.03 | 0.12 |
| 18113921−3652069 | +0.08 | +0.04 | +0.03 | −0.06 | 0.04 | 0.12 |
| 18111325−3646007 | +0.09 | +0.02 | +0.03 | −0.07 | 0.04 | 0.13 |
| 18113833−3626322 | +0.06 | +0.05 | +0.05 | −0.07 | 0.03 | 0.12 |
| 18111018−3639350 | +0.07 | +0.04 | +0.04 | −0.08 | 0.03 | 0.12 |
| 18135243−3630481 | +0.09 | +0.02 | +0.02 | −0.06 | 0.03 | 0.12 |
| 18121150−3627559 | +0.08 | +0.04 | +0.04 | −0.08 | 0.03 | 0.13 |
| 18111963−3647245 | +0.07 | +0.05 | +0.04 | −0.08 | 0.04 | 0.13 |
| 18140023−3635461 | +0.06 | +0.05 | +0.04 | −0.08 | 0.03 | 0.12 |
| 18135881−3639345 | +0.06 | +0.05 | +0.04 | −0.08 | 0.04 | 0.13 |
| 18121436−3654551 | +0.05 | +0.07 | +0.05 | −0.09 | 0.03 | 0.14 |
| 18124228−3655079 | +0.04 | +0.06 | +0.06 | −0.08 | 0.02 | 0.12 |
| 18122530−3637366 | +0.04 | +0.07 | +0.05 | −0.09 | 0.03 | 0.13 |
| 18131370−3651584 | +0.06 | +0.05 | +0.04 | −0.10 | 0.04 | 0.14 |
| 18134668−3623541 | +0.05 | +0.05 | +0.05 | −0.08 | 0.03 | 0.12 |
| 18105081−3642137 | +0.07 | +0.03 | +0.03 | −0.09 | 0.03 | 0.13 |
| 18124219−3631172 | +0.05 | +0.06 | +0.05 | −0.09 | 0.04 | 0.14 |
| 18133688−3647054 | +0.07 | +0.03 | +0.03 | −0.08 | 0.03 | 0.12 |
| 18123142−3639294 | +0.02 | +0.08 | +0.05 | −0.09 | 0.04 | 0.14 |
| 18133038−3632229 | +0.07 | +0.03 | +0.02 | −0.07 | 0.03 | 0.11 |
| 18133292−3624179 | +0.08 | +0.03 | +0.02 | −0.07 | 0.04 | 0.12 |
| 18111681−3636318 | +0.02 | +0.06 | +0.06 | −0.11 | 0.02 | 0.14 |
| 18105004−3640063 | +0.07 | +0.04 | +0.04 | −0.08 | 0.04 | 0.13 |
| 18112334−3634194 | +0.06 | +0.04 | +0.04 | −0.09 | 0.03 | 0.13 |
| 18131027−3632343 | +0.04 | +0.06 | +0.05 | −0.10 | 0.03 | 0.14 |
| 18110293−3628041 | +0.03 | +0.07 | +0.06 | −0.09 | 0.03 | 0.14 |
| 18132040−3623075 | +0.05 | +0.04 | +0.05 | −0.09 | 0.03 | 0.12 |
| 18135588−3629188 | +0.06 | +0.05 | +0.05 | −0.08 | 0.02 | 0.12 |
| 18105075−3635061 | +0.02 | +0.07 | +0.06 | −0.11 | 0.04 | 0.15 |
| 18104188−3634541 | +0.07 | +0.04 | +0.03 | −0.08 | 0.04 | 0.12 |
| 18132998−3628578 | +0.02 | +0.08 | +0.07 | −0.10 | 0.03 | 0.15 |
| 18130544−3616563 | +0.02 | +0.07 | +0.06 | −0.10 | 0.03 | 0.14 |
| 18115908−3654510 | +0.02 | +0.08 | +0.07 | −0.12 | 0.03 | 0.16 |
| 18121077−3639094 | +0.03 | +0.06 | +0.06 | −0.10 | 0.03 | 0.14 |
| 18120614−3629571 | +0.05 | +0.04 | +0.06 | −0.11 | 0.03 | 0.14 |
| 18120213−3641599 | +0.06 | +0.04 | +0.04 | −0.10 | 0.03 | 0.13 |
| 18123350−3654398 | +0.01 | +0.08 | +0.08 | −0.11 | 0.05 | 0.17 |
| 18120973−3654184 | +0.00 | +0.09 | +0.09 | −0.10 | 0.04 | 0.17 |
| 18105641−3632359 | +0.04 | +0.04 | +0.06 | −0.11 | 0.03 | 0.14 |
| 18125106−3654091 | +0.06 | +0.04 | +0.04 | −0.11 | 0.04 | 0.14 |
| 18111581−3648469 | +0.00 | +0.08 | +0.09 | −0.12 | 0.03 | 0.17 |
| 18131387−3630130 | +0.02 | +0.08 | +0.08 | −0.11 | 0.05 | 0.17 |
| 18123592−3634476 | +0.00 | +0.09 | +0.09 | −0.10 | 0.03 | 0.16 |
| 18135736−3638266 | +0.02 | +0.07 | +0.08 | −0.12 | 0.03 | 0.16 |
| 18133233−3626133 | +0.00 | +0.09 | +0.09 | −0.11 | 0.04 | 0.17 |
| 18125003−3630269 | +0.04 | +0.05 | +0.06 | −0.10 | 0.03 | 0.14 |
| 18130723−3618385 | +0.05 | +0.05 | +0.05 | −0.11 | 0.03 | 0.14 |
| 18125800−3616427 | +0.07 | +0.04 | +0.03 | −0.10 | 0.03 | 0.14 |
| 18111323−3637030 | +0.05 | +0.05 | +0.05 | −0.12 | 0.03 | 0.15 |
| 18130427−3630012 | +0.06 | +0.05 | +0.04 | −0.11 | 0.03 | 0.14 |
| 18124614−3617326 | +0.02 | +0.07 | +0.07 | −0.11 | 0.03 | 0.15 |
| 18120399−3615387 | +0.01 | +0.07 | +0.07 | −0.13 | 0.03 | 0.17 |
| 18123475−3624478 | +0.04 | +0.06 | +0.05 | −0.10 | 0.05 | 0.14 |
| 18115661−3617533 | +0.06 | +0.05 | +0.04 | −0.10 | 0.04 | 0.14 |
| 18113299−3623341 | +0.01 | +0.06 | +0.07 | −0.12 | 0.02 | 0.15 |
| 18111553−3628156 | +0.01 | +0.08 | +0.07 | −0.12 | 0.03 | 0.16 |
| 18125907−3644275 | +0.06 | +0.05 | +0.04 | −0.09 | 0.04 | 0.13 |
| 18111726−3620302 | +0.03 | +0.06 | +0.05 | −0.10 | 0.04 | 0.14 |
| 18111579−3625114 | −0.01 | +0.09 | +0.06 | −0.13 | 0.03 | 0.17 |
| 18131305−3650449 | +0.04 | +0.06 | +0.05 | −0.12 | 0.03 | 0.15 |
| 18123152−3636498 | −0.01 | +0.08 | +0.06 | −0.13 | 0.03 | 0.17 |
| 18125914−3619208 | +0.04 | +0.06 | +0.04 | −0.12 | 0.02 | 0.15 |
| 18115073−3650493 | +0.03 | +0.06 | +0.05 | −0.10 | 0.04 | 0.14 |
| 18114648−3625169 | +0.06 | +0.05 | +0.04 | −0.11 | 0.04 | 0.15 |
| 18113751−3629139 | −0.01 | +0.08 | +0.06 | −0.13 | 0.03 | 0.17 |
| 18122243−3637539 | +0.02 | +0.06 | +0.05 | −0.12 | 0.03 | 0.15 |
| 18133366−3644575 | +0.06 | +0.05 | +0.04 | −0.11 | 0.03 | 0.14 |
| 18134702−3641477 | +0.06 | +0.05 | +0.04 | −0.11 | 0.03 | 0.14 |
| 18125228−3618294 | +0.05 | +0.06 | +0.04 | −0.12 | 0.04 | 0.15 |
| 18110942−3647198 | +0.06 | +0.06 | +0.04 | −0.11 | 0.04 | 0.15 |
| 18104824−3638507 | −0.01 | +0.08 | +0.06 | −0.14 | 0.03 | 0.17 |
| 18122301−3629462 | −0.02 | +0.08 | +0.06 | −0.13 | 0.03 | 0.17 |
| 18133332−3645578 | −0.02 | +0.08 | +0.06 | −0.12 | 0.04 | 0.16 |
| 18123434−3652241 | +0.02 | +0.06 | +0.06 | −0.12 | 0.03 | 0.15 |
| 18112311−3625456 | +0.04 | +0.07 | +0.05 | −0.11 | 0.03 | 0.15 |
| 18125463−3649277 | +0.02 | +0.06 | +0.06 | −0.12 | 0.03 | 0.15 |
| 18123925−3620465 | −0.01 | +0.07 | +0.06 | −0.14 | 0.03 | 0.17 |
| 18110629−3632146 | +0.01 | +0.05 | +0.06 | −0.13 | 0.03 | 0.15 |
| 18133687−3639590 | +0.05 | +0.06 | +0.05 | −0.11 | 0.04 | 0.15 |
| 18111505−3620576 | +0.05 | +0.06 | +0.05 | −0.13 | 0.03 | 0.16 |
| 18120832−3628243 | +0.01 | +0.06 | +0.06 | −0.13 | 0.03 | 0.16 |
| 18130815−3631460 | −0.02 | +0.09 | +0.07 | −0.15 | 0.04 | 0.19 |
| 18120407−3636481 | −0.01 | +0.07 | +0.07 | −0.14 | 0.03 | 0.17 |
| 18135786−3640300 | +0.01 | +0.08 | +0.07 | −0.15 | 0.04 | 0.19 |
| 18131228−3619138 | +0.02 | +0.06 | +0.07 | −0.13 | 0.03 | 0.16 |
| 18113372−3650200 | +0.00 | +0.07 | +0.08 | −0.14 | 0.03 | 0.18 |
| 18115904−3650428 | −0.01 | +0.07 | +0.08 | −0.15 | 0.03 | 0.19 |
| 18115448−3641161 | +0.02 | +0.07 | +0.07 | −0.13 | 0.04 | 0.17 |
| 18123678−3649019 | +0.03 | +0.06 | +0.07 | −0.14 | 0.03 | 0.17 |
| 18113965−3645408 | +0.00 | +0.07 | +0.08 | −0.15 | 0.04 | 0.19 |
| 18135362−3636538 | +0.03 | +0.09 | +0.07 | −0.13 | 0.03 | 0.18 |
| 18123168−3631555 | +0.05 | +0.06 | +0.06 | −0.13 | 0.04 | 0.17 |
| 18115398−3623290 | −0.02 | +0.07 | +0.09 | −0.13 | 0.03 | 0.18 |
| 18123393−3615508 | +0.04 | +0.06 | +0.06 | −0.13 | 0.03 | 0.16 |
| 18120689−3643231 | +0.03 | +0.08 | +0.07 | −0.13 | 0.03 | 0.17 |
| 18130482−3649019 | −0.02 | +0.06 | +0.08 | −0.13 | 0.05 | 0.17 |
| 18110352−3646275 | −0.02 | +0.08 | +0.08 | −0.15 | 0.03 | 0.19 |
| 18105013−3629557 | +0.01 | +0.07 | +0.08 | −0.15 | 0.02 | 0.19 |
| 18121897−3630243 | +0.04 | +0.06 | +0.05 | −0.14 | 0.03 | 0.17 |
| 18122029−3652333 | +0.02 | +0.08 | +0.06 | −0.15 | 0.04 | 0.19 |
| (l, b) = (+8.5, +9) | ||||||
| 17311256−1702018 | +0.07 | +0.05 | +0.04 | −0.08 | 0.04 | 0.13 |
| 17290874−1632431 | +0.05 | +0.06 | +0.05 | −0.08 | 0.03 | 0.13 |
| 17302885−1639588 | +0.05 | +0.05 | +0.05 | −0.08 | 0.04 | 0.12 |
| 17304789−1623192 | +0.06 | +0.04 | +0.05 | −0.08 | 0.04 | 0.13 |
| 17321080−1641479 | +0.02 | +0.07 | +0.08 | −0.09 | 0.04 | 0.15 |
| 17303589−1638299 | +0.04 | +0.05 | +0.06 | −0.10 | 0.02 | 0.13 |
| 17290513−1630383 | +0.02 | +0.07 | +0.07 | −0.08 | 0.05 | 0.14 |
| 17314699−1654460 | +0.04 | +0.06 | +0.06 | −0.09 | 0.04 | 0.14 |
| 17305076−1615216 | +0.03 | +0.06 | +0.05 | −0.10 | 0.04 | 0.14 |
| 17323324−1627474 | +0.00 | +0.09 | +0.06 | −0.11 | 0.07 | 0.17 |
| 17312795−1631423 | +0.03 | +0.08 | +0.05 | −0.10 | 0.04 | 0.15 |
| 17290285−1638344 | +0.03 | +0.08 | +0.05 | −0.09 | 0.05 | 0.14 |
| 17303378−1703086 | +0.00 | +0.09 | +0.07 | −0.11 | 0.05 | 0.17 |
| 17304223−1609274 | +0.00 | +0.08 | +0.08 | −0.11 | 0.04 | 0.16 |
| 17304908−1633101 | +0.01 | +0.07 | +0.07 | −0.10 | 0.04 | 0.15 |
| 17291459−1650085 | +0.00 | +0.07 | +0.08 | −0.11 | 0.04 | 0.16 |
| 17300674−1638541 | +0.00 | +0.07 | +0.08 | −0.11 | 0.04 | 0.16 |
| 17315010−1653413 | +0.02 | +0.07 | +0.08 | −0.10 | 0.04 | 0.15 |
| 17295493−1613273 | +0.00 | +0.06 | +0.09 | −0.12 | 0.04 | 0.17 |
| 17311523−1618542 | +0.02 | +0.07 | +0.08 | −0.11 | 0.05 | 0.16 |
| 17314811−1621558 | +0.01 | +0.09 | +0.09 | −0.11 | 0.04 | 0.17 |
| 17304861−1646459 | −0.01 | +0.07 | +0.10 | −0.12 | 0.04 | 0.18 |
| 17323959−1625298 | +0.01 | +0.08 | +0.09 | −0.11 | 0.04 | 0.17 |
| 17285711−1633566 | +0.01 | +0.09 | +0.09 | −0.12 | 0.03 | 0.18 |
| 17314673−1641228 | −0.01 | +0.07 | +0.09 | −0.11 | 0.06 | 0.17 |
| 17294476−1626118 | −0.01 | +0.08 | +0.09 | −0.10 | 0.07 | 0.17 |
| 17320650−1643389 | −0.02 | +0.07 | +0.07 | −0.13 | 0.05 | 0.17 |
| 17314427−1640265 | +0.01 | +0.07 | +0.07 | −0.11 | 0.04 | 0.15 |
| 17300064−1701075 | −0.02 | +0.07 | +0.07 | −0.13 | 0.06 | 0.18 |
| 17302935−1652277 | +0.01 | +0.07 | +0.06 | −0.12 | 0.05 | 0.16 |
| 17320652−1619563 | −0.01 | +0.10 | +0.06 | −0.13 | 0.05 | 0.18 |
| 17304464−1631471 | −0.01 | +0.09 | +0.06 | −0.11 | 0.04 | 0.16 |
| 17321715−1632467 | −0.01 | +0.09 | +0.06 | −0.12 | 0.04 | 0.17 |
| 17321969−1653156 | −0.01 | +0.10 | +0.06 | −0.13 | 0.05 | 0.18 |
| 17315690−1630315 | −0.02 | +0.10 | +0.06 | −0.13 | 0.03 | 0.18 |
| 17312870−1619572 | −0.03 | +0.10 | +0.06 | −0.13 | 0.03 | 0.18 |
| 17294541−1649018 | −0.02 | +0.09 | +0.06 | −0.14 | 0.05 | 0.18 |
| 17305067−1644006 | −0.02 | +0.10 | +0.06 | −0.13 | 0.04 | 0.18 |
| 17312457−1652524 | −0.01 | +0.07 | +0.06 | −0.13 | 0.04 | 0.16 |
| 17292760−1636235 | −0.01 | +0.09 | +0.07 | −0.13 | 0.05 | 0.18 |
| 17295978−1633590 | −0.02 | +0.11 | +0.06 | −0.13 | 0.04 | 0.19 |
| 17322323−1649335 | −0.01 | +0.07 | +0.06 | −0.12 | 0.04 | 0.16 |
| 17321117−1654590 | −0.01 | +0.07 | +0.06 | −0.13 | 0.03 | 0.16 |
| 17313606−1607539 | +0.00 | +0.07 | +0.06 | −0.13 | 0.04 | 0.16 |
| 17295331−1653069 | −0.01 | +0.07 | +0.07 | −0.14 | 0.04 | 0.18 |
| 17302818−1636032 | −0.01 | +0.08 | +0.07 | −0.14 | 0.03 | 0.18 |
| 17293118−1638081 | −0.01 | +0.06 | +0.07 | −0.12 | 0.04 | 0.16 |
| 17291994−1618302 | −0.02 | +0.11 | +0.08 | −0.12 | 0.06 | 0.19 |
| 17320457−1646391 | −0.02 | +0.09 | +0.08 | −0.13 | 0.04 | 0.18 |
| 17310747−1620049 | −0.01 | +0.07 | +0.08 | −0.14 | 0.03 | 0.18 |
| 17323392−1636330 | −0.03 | +0.10 | +0.08 | −0.15 | 0.04 | 0.20 |
| 17312572−1609092 | +0.00 | +0.07 | +0.08 | −0.14 | 0.04 | 0.18 |
| 17300015−1609464 | −0.01 | +0.07 | +0.08 | −0.14 | 0.07 | 0.19 |
| 17305894−1637056 | −0.03 | +0.12 | +0.09 | −0.15 | 0.05 | 0.22 |
| 17291621−1647189 | −0.03 | +0.12 | +0.09 | −0.16 | 0.03 | 0.22 |
| 17302194−1643531 | −0.03 | +0.10 | +0.09 | −0.15 | 0.06 | 0.21 |
| 17311959−1643577 | −0.02 | +0.08 | +0.08 | −0.15 | 0.04 | 0.19 |
| 17311229−1659047 | −0.03 | +0.10 | +0.07 | −0.16 | 0.05 | 0.21 |
| 17313313−1659216 | −0.02 | +0.08 | +0.07 | −0.15 | 0.04 | 0.19 |
| 17301749−1629529 | −0.02 | +0.06 | +0.07 | −0.15 | 0.04 | 0.18 |
| 17294261−1622440 | −0.03 | +0.07 | +0.07 | −0.16 | 0.05 | 0.20 |
| 17323625−1637551 | −0.02 | +0.07 | +0.08 | −0.16 | 0.03 | 0.20 |
| 17314292−1620036 | −0.03 | +0.09 | +0.09 | −0.15 | 0.06 | 0.21 |
| 17310955−1635152 | −0.04 | +0.10 | +0.09 | −0.17 | 0.05 | 0.23 |
| 17304312−1630318 | −0.02 | +0.07 | +0.08 | −0.16 | 0.03 | 0.20 |
| 17285469−1627232 | −0.01 | +0.09 | +0.08 | −0.16 | 0.03 | 0.20 |
| 17310360−1700146 | −0.03 | +0.07 | +0.09 | −0.16 | 0.04 | 0.20 |
| 17295898−1652101 | −0.02 | +0.08 | +0.09 | −0.17 | 0.02 | 0.21 |
Table 6. Abundance Uncertainty: Oxygen
| Star ID | ΔTeff | Δlog(g) | Δ[M/H] | ΔVt | σ/√(N) | ΔTotal |
|---|---|---|---|---|---|---|
| 2MASS | (+100 K) | (+0.3 cgs) | (+0.3 dex) | (+0.3 km s-1) | ||
| (l, b) = (−5.5, −7) | ||||||
| 18011989−3723462 | +0.01 | +0.12 | +0.11 | −0.01 | 0.05 | 0.17 |
| 18003452−3729217 | ... | ... | ... | ... | ... | ... |
| 18011692−3722508 | +0.02 | +0.13 | +0.11 | −0.01 | 0.05 | 0.18 |
| 18005584−3739103 | +0.01 | +0.12 | +0.11 | −0.02 | 0.05 | 0.17 |
| 18015010−3735279 | +0.01 | +0.14 | +0.11 | −0.03 | 0.05 | 0.19 |
| 18005916−3727585 | +0.02 | +0.12 | +0.12 | −0.02 | 0.05 | 0.18 |
| 18005027−3707505 | +0.01 | +0.13 | +0.11 | −0.02 | 0.05 | 0.18 |
| 18005234−3715478 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18020106−3737561 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 17595541−3713447 | +0.02 | +0.12 | +0.11 | −0.02 | 0.05 | 0.17 |
| 17595664−3725304 | +0.01 | +0.13 | +0.11 | −0.01 | 0.05 | 0.18 |
| 18021345−3730371 | ... | ... | ... | ... | ... | ... |
| 17594241−3718247 | +0.01 | +0.13 | +0.11 | −0.02 | 0.05 | 0.18 |
| 18013342−3726339 | ... | ... | ... | ... | ... | ... |
| 18003204−3726008 | +0.02 | +0.12 | +0.10 | −0.06 | 0.05 | 0.18 |
| 18013580−3740055 | +0.02 | +0.13 | +0.11 | −0.02 | 0.05 | 0.18 |
| 18013799−3725131 | +0.02 | +0.13 | +0.10 | −0.05 | 0.05 | 0.18 |
| 18022149−3713494 | ... | ... | ... | ... | ... | ... |
| 18011408−3711299 | +0.01 | +0.14 | +0.11 | −0.02 | 0.05 | 0.19 |
| 18021275−3737543 | ... | ... | ... | ... | ... | ... |
| 17595027−3727293 | ... | ... | ... | ... | ... | ... |
| 18002115−3715519 | +0.02 | +0.12 | +0.12 | −0.04 | 0.05 | 0.18 |
| 17595366−3728186 | ... | ... | ... | ... | ... | ... |
| 18001354−3709122 | +0.02 | +0.14 | +0.12 | −0.03 | 0.05 | 0.19 |
| 18013960−3723398 | +0.02 | +0.14 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18021862−3734204 | ... | ... | ... | ... | ... | ... |
| 18000535−3735315 | +0.02 | +0.13 | +0.12 | −0.03 | 0.05 | 0.19 |
| 18013848−3721442 | +0.02 | +0.13 | +0.12 | −0.04 | 0.05 | 0.19 |
| 17594792−3721422 | ... | ... | ... | ... | ... | ... |
| 18011941−3721250 | ... | ... | ... | ... | ... | ... |
| 18004824−3718074 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18014343−3708232 | +0.02 | +0.14 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18005852−3711524 | +0.01 | +0.14 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18020816−3714015 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18010932−3702079 | +0.02 | +0.13 | +0.13 | −0.02 | 0.05 | 0.19 |
| 18010065−3740456 | +0.02 | +0.14 | +0.13 | −0.05 | 0.05 | 0.20 |
| 17595640−3710383 | +0.02 | +0.12 | +0.12 | −0.02 | 0.05 | 0.18 |
| 18012462−3738382 | +0.02 | +0.13 | +0.11 | −0.03 | 0.05 | 0.18 |
| 18002880−3710171 | +0.01 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18024484−3714159 | +0.01 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18013206−3708133 | ... | ... | ... | ... | ... | ... |
| 18004074−3740058 | +0.02 | +0.12 | +0.11 | −0.01 | 0.05 | 0.17 |
| 18000013−3715053 | +0.02 | +0.12 | +0.11 | −0.02 | 0.05 | 0.17 |
| 18015431−3717070 | +0.02 | +0.13 | +0.11 | −0.02 | 0.05 | 0.18 |
| 18021006−3738193 | +0.01 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 17595442−3721118 | +0.02 | +0.12 | +0.11 | −0.02 | 0.05 | 0.17 |
| 18021721−3736096 | +0.01 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18005096−3733499 | +0.02 | +0.11 | +0.10 | −0.05 | 0.05 | 0.17 |
| 18005923−3707111 | ... | ... | ... | ... | ... | ... |
| 18011851−3706092 | +0.02 | +0.12 | +0.11 | −0.03 | 0.05 | 0.17 |
| 18013395−3705551 | +0.02 | +0.13 | +0.11 | −0.02 | 0.05 | 0.18 |
| 18022648−3728188 | +0.01 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18024919−3727234 | +0.01 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18023660−3716289 | +0.01 | +0.14 | +0.12 | −0.02 | 0.05 | 0.19 |
| 17595509−3711099 | ... | ... | ... | ... | ... | ... |
| 18005395−3731231 | +0.02 | +0.12 | +0.12 | −0.01 | 0.05 | 0.18 |
| 18010322−3705447 | +0.01 | +0.13 | +0.13 | −0.01 | 0.05 | 0.19 |
| 18014769−3739220 | +0.02 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 17594807−3715283 | +0.01 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18013618−3706311 | +0.02 | +0.11 | +0.12 | −0.02 | 0.05 | 0.17 |
| 18004314−3730156 | ... | ... | ... | ... | ... | ... |
| 18014303−3740054 | ... | ... | ... | ... | ... | ... |
| 18003751−3728200 | +0.02 | +0.13 | +0.13 | −0.02 | 0.05 | 0.19 |
| 18011170−3727118 | ... | ... | ... | ... | ... | ... |
| 18023846−3718345 | ... | ... | ... | ... | ... | ... |
| 18011671−3722213 | +0.01 | +0.14 | +0.13 | −0.01 | 0.05 | 0.20 |
| 18005985−3734507 | ... | ... | ... | ... | ... | ... |
| 18000430−3711051 | +0.02 | +0.11 | +0.12 | −0.04 | 0.05 | 0.18 |
| 18003552−3729476 | ... | ... | ... | ... | ... | ... |
| 18001817−3732243 | ... | ... | ... | ... | ... | ... |
| 18013039−3713086 | +0.02 | +0.12 | +0.13 | −0.01 | 0.05 | 0.19 |
| 18012564−3741052 | +0.02 | +0.13 | +0.13 | −0.02 | 0.05 | 0.19 |
| 18025713−3718318 | ... | ... | ... | ... | ... | ... |
| 18011599−3741385 | +0.02 | +0.12 | +0.13 | −0.02 | 0.05 | 0.19 |
| 18012944−3719488 | ... | ... | ... | ... | ... | ... |
| 18020361−3719086 | +0.02 | +0.14 | +0.13 | −0.01 | 0.05 | 0.20 |
| 18024024−3728187 | +0.02 | +0.12 | +0.13 | −0.01 | 0.05 | 0.19 |
| 18000412−3717266 | +0.02 | +0.12 | +0.13 | −0.01 | 0.05 | 0.19 |
| 18011177−3703344 | +0.02 | +0.12 | +0.13 | −0.01 | 0.05 | 0.19 |
| 18001410−3725181 | +0.02 | +0.12 | +0.13 | −0.02 | 0.05 | 0.19 |
| 18020300−3719418 | +0.02 | +0.12 | +0.12 | −0.02 | 0.05 | 0.18 |
| 18004683−3703252 | +0.02 | +0.12 | +0.12 | −0.03 | 0.05 | 0.18 |
| 18015404−3722564 | +0.02 | +0.12 | +0.12 | −0.04 | 0.05 | 0.18 |
| 18013974−3704068 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18020704−3708064 | +0.02 | +0.14 | +0.13 | −0.01 | 0.05 | 0.20 |
| 18023393−3730273 | ... | ... | ... | ... | ... | ... |
| 18001720−3708374 | +0.02 | +0.12 | +0.13 | −0.01 | 0.05 | 0.19 |
| 18003663−3708547 | ... | ... | ... | ... | ... | ... |
| 18002569−3729578 | +0.02 | +0.14 | +0.13 | −0.01 | 0.05 | 0.20 |
| 17594881−3716203 | +0.01 | +0.13 | +0.13 | −0.04 | 0.05 | 0.19 |
| 18011201−3740090 | +0.02 | +0.14 | +0.13 | −0.01 | 0.05 | 0.20 |
| (l, b) = (−4, −9) | ||||||
| 18122552−3653049 | +0.02 | +0.13 | +0.10 | −0.01 | 0.05 | 0.17 |
| 18120653−3654264 | ... | ... | ... | ... | ... | ... |
| 18110179−3630394 | +0.02 | +0.12 | +0.11 | −0.01 | 0.05 | 0.17 |
| 18124892−3626403 | +0.01 | +0.12 | +0.10 | −0.01 | 0.05 | 0.16 |
| 18135164−3643463 | +0.02 | +0.12 | +0.11 | −0.01 | 0.05 | 0.17 |
| 18124339−3635339 | +0.02 | +0.12 | +0.11 | −0.01 | 0.05 | 0.17 |
| 18113921−3652069 | ... | ... | ... | ... | ... | ... |
| 18111325−3646007 | +0.02 | +0.13 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18113833−3626322 | +0.03 | +0.12 | +0.12 | −0.03 | 0.05 | 0.18 |
| 18111018−3639350 | +0.02 | +0.13 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18135243−3630481 | +0.01 | +0.13 | +0.12 | −0.01 | 0.05 | 0.18 |
| 18121150−3627559 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18111963−3647245 | +0.02 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18140023−3635461 | +0.02 | +0.14 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18135881−3639345 | +0.02 | +0.14 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18121436−3654551 | +0.02 | +0.14 | +0.11 | −0.03 | 0.05 | 0.19 |
| 18124228−3655079 | +0.02 | +0.13 | +0.11 | −0.04 | 0.05 | 0.18 |
| 18122530−3637366 | +0.02 | +0.14 | +0.11 | −0.02 | 0.05 | 0.19 |
| 18131370−3651584 | ... | ... | ... | ... | ... | ... |
| 18134668−3623541 | ... | ... | ... | ... | ... | ... |
| 18105081−3642137 | +0.02 | +0.13 | +0.11 | −0.01 | 0.05 | 0.18 |
| 18124219−3631172 | +0.02 | +0.13 | +0.11 | −0.02 | 0.05 | 0.18 |
| 18133688−3647054 | ... | ... | ... | ... | ... | ... |
| 18123142−3639294 | +0.02 | +0.14 | +0.10 | −0.03 | 0.05 | 0.18 |
| 18133038−3632229 | ... | ... | ... | ... | ... | ... |
| 18133292−3624179 | +0.01 | +0.14 | +0.11 | −0.01 | 0.05 | 0.19 |
| 18111681−3636318 | +0.02 | +0.11 | +0.10 | −0.03 | 0.05 | 0.16 |
| 18105004−3640063 | +0.02 | +0.12 | +0.11 | −0.01 | 0.05 | 0.17 |
| 18112334−3634194 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18131027−3632343 | +0.02 | +0.13 | +0.11 | −0.02 | 0.05 | 0.18 |
| 18110293−3628041 | +0.02 | +0.13 | +0.11 | −0.04 | 0.05 | 0.18 |
| 18132040−3623075 | +0.01 | +0.11 | +0.11 | −0.03 | 0.05 | 0.17 |
| 18135588−3629188 | +0.02 | +0.12 | +0.11 | −0.03 | 0.05 | 0.17 |
| 18105075−3635061 | +0.02 | +0.13 | +0.11 | −0.03 | 0.05 | 0.18 |
| 18104188−3634541 | +0.01 | +0.14 | +0.11 | −0.02 | 0.05 | 0.19 |
| 18132998−3628578 | +0.02 | +0.13 | +0.11 | −0.04 | 0.05 | 0.18 |
| 18130544−3616563 | ... | ... | ... | ... | ... | ... |
| 18115908−3654510 | +0.02 | +0.14 | +0.11 | −0.02 | 0.05 | 0.19 |
| 18121077−3639094 | +0.02 | +0.12 | +0.12 | −0.02 | 0.05 | 0.18 |
| 18120614−3629571 | +0.01 | +0.12 | +0.12 | −0.01 | 0.05 | 0.18 |
| 18120213−3641599 | ... | ... | ... | ... | ... | ... |
| 18123350−3654398 | ... | ... | ... | ... | ... | ... |
| 18120973−3654184 | +0.02 | +0.13 | +0.12 | −0.05 | 0.05 | 0.19 |
| 18105641−3632359 | +0.02 | +0.12 | +0.12 | −0.01 | 0.05 | 0.18 |
| 18125106−3654091 | +0.01 | +0.13 | +0.12 | −0.01 | 0.05 | 0.18 |
| 18111581−3648469 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18131387−3630130 | ... | ... | ... | ... | ... | ... |
| 18123592−3634476 | +0.03 | +0.13 | +0.13 | −0.02 | 0.05 | 0.19 |
| 18135736−3638266 | +0.02 | +0.12 | +0.12 | −0.02 | 0.05 | 0.18 |
| 18133233−3626133 | +0.02 | +0.13 | +0.13 | −0.03 | 0.05 | 0.19 |
| 18125003−3630269 | +0.02 | +0.12 | +0.12 | −0.01 | 0.05 | 0.18 |
| 18130723−3618385 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18125800−3616427 | +0.02 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18111323−3637030 | +0.01 | +0.13 | +0.12 | −0.01 | 0.05 | 0.18 |
| 18130427−3630012 | +0.01 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18124614−3617326 | ... | ... | ... | ... | ... | ... |
| 18120399−3615387 | +0.02 | +0.12 | +0.12 | −0.02 | 0.05 | 0.18 |
| 18123475−3624478 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18115661−3617533 | +0.01 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18113299−3623341 | +0.02 | +0.12 | +0.11 | −0.02 | 0.05 | 0.17 |
| 18111553−3628156 | +0.02 | +0.13 | +0.11 | −0.04 | 0.05 | 0.18 |
| 18125907−3644275 | +0.01 | +0.13 | +0.12 | −0.01 | 0.05 | 0.18 |
| 18111726−3620302 | +0.02 | +0.13 | +0.11 | −0.01 | 0.05 | 0.18 |
| 18111579−3625114 | +0.02 | +0.13 | +0.11 | −0.04 | 0.05 | 0.18 |
| 18131305−3650449 | ... | ... | ... | ... | ... | ... |
| 18123152−3636498 | +0.02 | +0.12 | +0.11 | −0.02 | 0.05 | 0.17 |
| 18125914−3619208 | +0.01 | +0.14 | +0.11 | −0.01 | 0.05 | 0.19 |
| 18115073−3650493 | ... | ... | ... | ... | ... | ... |
| 18114648−3625169 | ... | ... | ... | ... | ... | ... |
| 18113751−3629139 | ... | ... | ... | ... | ... | ... |
| 18122243−3637539 | +0.02 | +0.12 | +0.11 | −0.02 | 0.05 | 0.17 |
| 18133366−3644575 | +0.01 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18134702−3641477 | +0.01 | +0.14 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18125228−3618294 | +0.01 | +0.14 | +0.12 | +0.00 | 0.05 | 0.19 |
| 18110942−3647198 | ... | ... | ... | ... | ... | ... |
| 18104824−3638507 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18122301−3629462 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18133332−3645578 | +0.02 | +0.13 | +0.11 | −0.03 | 0.05 | 0.18 |
| 18123434−3652241 | +0.02 | +0.12 | +0.11 | −0.03 | 0.05 | 0.17 |
| 18112311−3625456 | +0.01 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18125463−3649277 | +0.02 | +0.12 | +0.11 | −0.04 | 0.05 | 0.18 |
| 18123925−3620465 | ... | ... | ... | ... | ... | ... |
| 18110629−3632146 | +0.02 | +0.12 | +0.12 | −0.01 | 0.05 | 0.18 |
| 18133687−3639590 | +0.01 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18111505−3620576 | +0.01 | +0.14 | +0.13 | −0.01 | 0.05 | 0.20 |
| 18120832−3628243 | +0.02 | +0.12 | +0.12 | −0.02 | 0.05 | 0.18 |
| 18130815−3631460 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 18120407−3636481 | +0.01 | +0.12 | +0.11 | −0.03 | 0.05 | 0.17 |
| 18135786−3640300 | +0.02 | +0.14 | +0.12 | −0.01 | 0.05 | 0.19 |
| 18131228−3619138 | +0.02 | +0.13 | +0.13 | −0.01 | 0.05 | 0.19 |
| 18113372−3650200 | +0.02 | +0.12 | +0.12 | −0.02 | 0.05 | 0.18 |
| 18115904−3650428 | ... | ... | ... | ... | ... | ... |
| 18115448−3641161 | +0.02 | +0.13 | +0.13 | −0.01 | 0.05 | 0.19 |
| 18123678−3649019 | +0.02 | +0.13 | +0.12 | −0.03 | 0.05 | 0.19 |
| 18113965−3645408 | ... | ... | ... | ... | ... | ... |
| 18135362−3636538 | ... | ... | ... | ... | ... | ... |
| 18123168−3631555 | +0.01 | +0.13 | +0.13 | −0.01 | 0.05 | 0.19 |
| 18115398−3623290 | +0.01 | +0.12 | +0.13 | −0.05 | 0.05 | 0.19 |
| 18123393−3615508 | ... | ... | ... | ... | ... | ... |
| 18120689−3643231 | +0.02 | +0.14 | +0.13 | −0.01 | 0.05 | 0.20 |
| 18130482−3649019 | +0.02 | +0.12 | +0.13 | −0.02 | 0.05 | 0.19 |
| 18110352−3646275 | +0.02 | +0.13 | +0.13 | −0.02 | 0.05 | 0.19 |
| 18105013−3629557 | +0.02 | +0.13 | +0.13 | −0.01 | 0.05 | 0.19 |
| 18121897−3630243 | ... | ... | ... | ... | ... | ... |
| 18122029−3652333 | ... | ... | ... | ... | ... | ... |
| (l, b) = (+8.5, +9) | ||||||
| 17311256−1702018 | +0.02 | +0.12 | +0.11 | −0.03 | 0.05 | 0.17 |
| 17290874−1632431 | +0.01 | +0.13 | +0.11 | −0.03 | 0.05 | 0.18 |
| 17302885−1639588 | +0.02 | +0.12 | +0.12 | −0.02 | 0.05 | 0.18 |
| 17304789−1623192 | +0.02 | +0.11 | +0.12 | −0.02 | 0.05 | 0.17 |
| 17321080−1641479 | +0.02 | +0.12 | +0.12 | −0.04 | 0.05 | 0.18 |
| 17303589−1638299 | +0.03 | +0.12 | +0.12 | −0.03 | 0.05 | 0.18 |
| 17290513−1630383 | +0.03 | +0.12 | +0.12 | −0.04 | 0.05 | 0.18 |
| 17314699−1654460 | +0.02 | +0.13 | +0.11 | −0.04 | 0.05 | 0.18 |
| 17305076−1615216 | +0.02 | +0.12 | +0.10 | −0.04 | 0.05 | 0.17 |
| 17323324−1627474 | +0.02 | +0.13 | +0.11 | −0.03 | 0.05 | 0.18 |
| 17312795−1631423 | +0.02 | +0.14 | +0.11 | −0.02 | 0.05 | 0.19 |
| 17290285−1638344 | +0.02 | +0.14 | +0.11 | −0.02 | 0.05 | 0.19 |
| 17303378−1703086 | +0.03 | +0.13 | +0.11 | −0.04 | 0.05 | 0.18 |
| 17304223−1609274 | +0.02 | +0.13 | +0.12 | −0.04 | 0.05 | 0.19 |
| 17304908−1633101 | ... | ... | ... | ... | ... | ... |
| 17291459−1650085 | +0.03 | +0.12 | +0.12 | −0.03 | 0.05 | 0.18 |
| 17300674−1638541 | ... | ... | ... | ... | ... | ... |
| 17315010−1653413 | +0.02 | +0.12 | +0.12 | −0.03 | 0.05 | 0.18 |
| 17295493−1613273 | ... | ... | ... | ... | ... | ... |
| 17311523−1618542 | ... | ... | ... | ... | ... | ... |
| 17314811−1621558 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 17304861−1646459 | +0.03 | +0.11 | +0.14 | −0.04 | 0.05 | 0.19 |
| 17323959−1625298 | ... | ... | ... | ... | ... | ... |
| 17285711−1633566 | +0.03 | +0.13 | +0.13 | −0.03 | 0.05 | 0.20 |
| 17314673−1641228 | +0.03 | +0.11 | +0.13 | −0.03 | 0.05 | 0.18 |
| 17294476−1626118 | +0.02 | +0.12 | +0.13 | −0.03 | 0.05 | 0.19 |
| 17320650−1643389 | +0.02 | +0.12 | +0.12 | −0.03 | 0.05 | 0.18 |
| 17314427−1640265 | +0.02 | +0.12 | +0.11 | −0.03 | 0.05 | 0.17 |
| 17300064−1701075 | ... | ... | ... | ... | ... | ... |
| 17302935−1652277 | +0.02 | +0.12 | +0.12 | −0.01 | 0.05 | 0.18 |
| 17320652−1619563 | +0.02 | +0.14 | +0.11 | −0.02 | 0.05 | 0.19 |
| 17304464−1631471 | +0.02 | +0.13 | +0.10 | −0.05 | 0.05 | 0.18 |
| 17321715−1632467 | ... | ... | ... | ... | ... | ... |
| 17321969−1653156 | +0.02 | +0.14 | +0.10 | −0.05 | 0.05 | 0.19 |
| 17315690−1630315 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 17312870−1619572 | +0.02 | +0.13 | +0.12 | −0.03 | 0.05 | 0.19 |
| 17294541−1649018 | +0.02 | +0.13 | +0.11 | −0.04 | 0.05 | 0.18 |
| 17305067−1644006 | +0.02 | +0.14 | +0.12 | −0.03 | 0.05 | 0.19 |
| 17312457−1652524 | +0.02 | +0.12 | +0.11 | −0.04 | 0.05 | 0.18 |
| 17292760−1636235 | +0.02 | +0.13 | +0.11 | −0.06 | 0.05 | 0.19 |
| 17295978−1633590 | ... | ... | ... | ... | ... | ... |
| 17322323−1649335 | +0.02 | +0.12 | +0.11 | −0.03 | 0.05 | 0.17 |
| 17321117−1654590 | +0.02 | +0.12 | +0.12 | −0.02 | 0.05 | 0.18 |
| 17313606−1607539 | +0.02 | +0.12 | +0.11 | −0.03 | 0.05 | 0.17 |
| 17295331−1653069 | +0.02 | +0.12 | +0.11 | −0.04 | 0.05 | 0.18 |
| 17302818−1636032 | +0.02 | +0.13 | +0.11 | −0.03 | 0.05 | 0.18 |
| 17293118−1638081 | ... | ... | ... | ... | ... | ... |
| 17291994−1618302 | +0.02 | +0.14 | +0.12 | −0.03 | 0.05 | 0.19 |
| 17320457−1646391 | +0.02 | +0.13 | +0.12 | −0.02 | 0.05 | 0.19 |
| 17310747−1620049 | +0.02 | +0.12 | +0.12 | −0.04 | 0.05 | 0.18 |
| 17323392−1636330 | +0.02 | +0.13 | +0.13 | −0.02 | 0.05 | 0.19 |
| 17312572−1609092 | +0.02 | +0.12 | +0.13 | −0.01 | 0.05 | 0.19 |
| 17300015−1609464 | ... | ... | ... | ... | ... | ... |
| 17305894−1637056 | +0.01 | +0.15 | +0.13 | −0.05 | 0.05 | 0.21 |
| 17291621−1647189 | +0.02 | +0.15 | +0.13 | −0.04 | 0.05 | 0.21 |
| 17302194−1643531 | +0.01 | +0.14 | +0.12 | −0.04 | 0.05 | 0.20 |
| 17311959−1643577 | ... | ... | ... | ... | ... | ... |
| 17311229−1659047 | ... | ... | ... | ... | ... | ... |
| 17313313−1659216 | +0.02 | +0.12 | +0.12 | −0.03 | 0.05 | 0.18 |
| 17301749−1629529 | +0.02 | +0.12 | +0.12 | −0.02 | 0.05 | 0.18 |
| 17294261−1622440 | ... | ... | ... | ... | ... | ... |
| 17323625−1637551 | +0.02 | +0.12 | +0.13 | −0.01 | 0.05 | 0.19 |
| 17314292−1620036 | ... | ... | ... | ... | ... | ... |
| 17310955−1635152 | +0.02 | +0.13 | +0.13 | −0.02 | 0.05 | 0.19 |
| 17304312−1630318 | ... | ... | ... | ... | ... | ... |
| 17285469−1627232 | +0.02 | +0.13 | +0.13 | −0.02 | 0.05 | 0.19 |
| 17310360−1700146 | ... | ... | ... | ... | ... | ... |
| 17295898−1652101 | +0.01 | +0.13 | +0.13 | −0.02 | 0.05 | 0.19 |
Table 7. Abundance Uncertainty: Silicon
| Star ID | ΔTeff | Δlog(g) | Δ[M/H] | ΔVt | σ/√(N) | ΔTotal |
|---|---|---|---|---|---|---|
| 2MASS | (+100 K) | (+0.3 cgs) | (+0.3 dex) | (+0.3 km s-1) | ||
| (l, b) = (−5.5, −7) | ||||||
| 18011989−3723462 | −0.02 | +0.03 | +0.04 | −0.01 | 0.05 | 0.07 |
| 18003452−3729217 | +0.00 | +0.04 | +0.03 | −0.01 | 0.05 | 0.07 |
| 18011692−3722508 | +0.00 | +0.06 | +0.04 | −0.01 | 0.05 | 0.09 |
| 18005584−3739103 | ... | ... | ... | ... | ... | ... |
| 18015010−3735279 | −0.03 | +0.08 | +0.05 | −0.02 | 0.12 | 0.16 |
| 18005916−3727585 | −0.02 | +0.04 | +0.06 | −0.02 | 0.05 | 0.09 |
| 18005027−3707505 | −0.02 | +0.06 | +0.05 | −0.02 | 0.03 | 0.09 |
| 18005234−3715478 | −0.05 | +0.07 | +0.06 | −0.02 | 0.05 | 0.12 |
| 18020106−3737561 | −0.05 | +0.08 | +0.06 | −0.02 | 0.05 | 0.12 |
| 17595541−3713447 | ... | ... | ... | ... | ... | ... |
| 17595664−3725304 | −0.03 | +0.06 | +0.05 | −0.03 | 0.05 | 0.10 |
| 18021345−3730371 | −0.08 | +0.09 | +0.04 | −0.03 | 0.03 | 0.13 |
| 17594241−3718247 | −0.06 | +0.07 | +0.05 | −0.03 | 0.05 | 0.12 |
| 18013342−3726339 | −0.04 | +0.05 | +0.05 | −0.03 | 0.05 | 0.10 |
| 18003204−3726008 | −0.09 | +0.07 | +0.05 | −0.03 | 0.00 | 0.13 |
| 18013580−3740055 | −0.09 | +0.09 | +0.05 | −0.03 | 0.06 | 0.15 |
| 18013799−3725131 | −0.09 | +0.09 | +0.05 | −0.04 | 0.02 | 0.14 |
| 18022149−3713494 | −0.08 | +0.10 | +0.05 | −0.03 | 0.05 | 0.15 |
| 18011408−3711299 | −0.04 | +0.08 | +0.06 | −0.04 | 0.01 | 0.12 |
| 18021275−3737543 | ... | ... | ... | ... | ... | ... |
| 17595027−3727293 | −0.07 | +0.08 | +0.06 | −0.03 | 0.05 | 0.14 |
| 18002115−3715519 | −0.10 | +0.08 | +0.07 | −0.03 | 0.04 | 0.15 |
| 17595366−3728186 | −0.04 | +0.07 | +0.07 | −0.04 | 0.05 | 0.12 |
| 18001354−3709122 | −0.09 | +0.13 | +0.08 | −0.04 | 0.05 | 0.19 |
| 18013960−3723398 | −0.09 | +0.12 | +0.07 | −0.04 | 0.08 | 0.19 |
| 18021862−3734204 | ... | ... | ... | ... | ... | ... |
| 18000535−3735315 | −0.09 | +0.10 | +0.07 | −0.04 | 0.02 | 0.16 |
| 18013848−3721442 | −0.08 | +0.11 | +0.08 | −0.03 | 0.05 | 0.17 |
| 17594792−3721422 | −0.07 | +0.05 | +0.07 | −0.04 | 0.01 | 0.12 |
| 18011941−3721250 | ... | ... | ... | ... | ... | ... |
| 18004824−3718074 | −0.10 | +0.10 | +0.08 | −0.03 | 0.05 | 0.17 |
| 18014343−3708232 | −0.09 | +0.12 | +0.08 | −0.03 | 0.10 | 0.20 |
| 18005852−3711524 | −0.04 | +0.08 | +0.07 | −0.05 | 0.02 | 0.13 |
| 18020816−3714015 | −0.04 | +0.07 | +0.07 | −0.04 | 0.14 | 0.18 |
| 18010932−3702079 | −0.09 | +0.12 | +0.08 | −0.03 | 0.19 | 0.26 |
| 18010065−3740456 | −0.09 | +0.12 | +0.09 | −0.04 | 0.05 | 0.19 |
| 17595640−3710383 | −0.08 | +0.05 | +0.06 | −0.04 | 0.05 | 0.13 |
| 18012462−3738382 | −0.05 | +0.08 | +0.07 | −0.04 | 0.05 | 0.13 |
| 18002880−3710171 | −0.04 | +0.09 | +0.05 | −0.04 | 0.05 | 0.13 |
| 18024484−3714159 | −0.04 | +0.09 | +0.05 | −0.03 | 0.05 | 0.12 |
| 18013206−3708133 | ... | ... | ... | ... | ... | ... |
| 18004074−3740058 | −0.07 | +0.06 | +0.05 | −0.03 | 0.05 | 0.12 |
| 18000013−3715053 | −0.08 | +0.07 | +0.04 | −0.04 | 0.02 | 0.12 |
| 18015431−3717070 | −0.06 | +0.09 | +0.05 | −0.04 | 0.13 | 0.18 |
| 18021006−3738193 | −0.04 | +0.08 | +0.05 | −0.03 | 0.08 | 0.13 |
| 17595442−3721118 | −0.09 | +0.09 | +0.03 | −0.05 | 0.14 | 0.20 |
| 18021721−3736096 | −0.04 | +0.10 | +0.05 | −0.03 | 0.05 | 0.13 |
| 18005096−3733499 | −0.09 | +0.05 | +0.04 | −0.05 | 0.05 | 0.13 |
| 18005923−3707111 | −0.10 | +0.07 | +0.03 | −0.04 | 0.09 | 0.16 |
| 18011851−3706092 | −0.10 | +0.07 | +0.03 | −0.04 | 0.00 | 0.13 |
| 18013395−3705551 | −0.10 | +0.09 | +0.03 | −0.05 | 0.02 | 0.15 |
| 18022648−3728188 | −0.05 | +0.10 | +0.05 | −0.04 | 0.26 | 0.29 |
| 18024919−3727234 | −0.05 | +0.10 | +0.05 | −0.04 | 0.14 | 0.19 |
| 18023660−3716289 | −0.05 | +0.10 | +0.05 | −0.06 | 0.05 | 0.15 |
| 17595509−3711099 | −0.07 | +0.08 | +0.05 | −0.03 | 0.05 | 0.13 |
| 18005395−3731231 | −0.10 | +0.10 | +0.03 | −0.04 | 0.06 | 0.16 |
| 18010322−3705447 | −0.05 | +0.09 | +0.05 | −0.04 | 0.05 | 0.13 |
| 18014769−3739220 | ... | ... | ... | ... | ... | ... |
| 17594807−3715283 | −0.05 | +0.11 | +0.05 | −0.04 | 0.05 | 0.15 |
| 18013618−3706311 | −0.09 | +0.05 | +0.05 | −0.05 | 0.04 | 0.13 |
| 18004314−3730156 | −0.05 | +0.11 | +0.07 | −0.04 | 0.02 | 0.15 |
| 18014303−3740054 | −0.08 | +0.07 | +0.06 | −0.04 | 0.05 | 0.14 |
| 18003751−3728200 | −0.10 | +0.12 | +0.06 | −0.04 | 0.02 | 0.17 |
| 18011170−3727118 | −0.03 | +0.08 | +0.06 | −0.03 | 0.05 | 0.12 |
| 18023846−3718345 | −0.08 | +0.09 | +0.07 | −0.03 | 0.05 | 0.15 |
| 18011671−3722213 | −0.04 | +0.08 | +0.07 | −0.04 | 0.05 | 0.13 |
| 18005985−3734507 | ... | ... | ... | ... | ... | ... |
| 18000430−3711051 | −0.09 | +0.06 | +0.07 | −0.05 | 0.08 | 0.16 |
| 18003552−3729476 | −0.08 | +0.08 | +0.07 | −0.04 | 0.00 | 0.14 |
| 18001817−3732243 | −0.06 | +0.10 | +0.07 | −0.05 | 0.05 | 0.15 |
| 18013039−3713086 | −0.09 | +0.09 | +0.07 | −0.04 | 0.01 | 0.15 |
| 18012564−3741052 | −0.08 | +0.10 | +0.07 | −0.04 | 0.09 | 0.18 |
| 18025713−3718318 | −0.09 | +0.10 | +0.06 | −0.04 | 0.06 | 0.16 |
| 18011599−3741385 | −0.09 | +0.08 | +0.07 | −0.06 | 0.06 | 0.16 |
| 18012944−3719488 | −0.04 | +0.09 | +0.06 | −0.04 | 0.05 | 0.13 |
| 18020361−3719086 | −0.07 | +0.11 | +0.07 | −0.06 | 0.05 | 0.17 |
| 18024024−3728187 | −0.10 | +0.07 | +0.06 | −0.04 | 0.04 | 0.15 |
| 18000412−3717266 | −0.10 | +0.06 | +0.05 | −0.04 | 0.02 | 0.13 |
| 18011177−3703344 | −0.08 | +0.09 | +0.06 | −0.03 | 0.14 | 0.20 |
| 18001410−3725181 | −0.10 | +0.08 | +0.05 | −0.04 | 0.11 | 0.18 |
| 18020300−3719418 | −0.10 | +0.06 | +0.04 | −0.04 | 0.12 | 0.18 |
| 18004683−3703252 | −0.10 | +0.09 | +0.04 | −0.04 | 0.15 | 0.21 |
| 18015404−3722564 | −0.08 | +0.08 | +0.04 | −0.03 | 0.02 | 0.13 |
| 18013974−3704068 | −0.08 | +0.09 | +0.06 | −0.04 | 0.08 | 0.16 |
| 18020704−3708064 | −0.05 | +0.11 | +0.06 | −0.04 | 0.05 | 0.15 |
| 18023393−3730273 | ... | ... | ... | ... | ... | ... |
| 18001720−3708374 | −0.10 | +0.07 | +0.06 | −0.03 | 0.05 | 0.15 |
| 18003663−3708547 | −0.08 | +0.10 | +0.06 | −0.04 | 0.00 | 0.15 |
| 18002569−3729578 | −0.06 | +0.13 | +0.06 | −0.04 | 0.05 | 0.17 |
| 17594881−3716203 | −0.09 | +0.12 | +0.06 | −0.04 | 0.02 | 0.17 |
| 18011201−3740090 | −0.06 | +0.13 | +0.06 | −0.06 | 0.05 | 0.17 |
| (l, b) = (−4, −9) | ||||||
| 18122552−3653049 | +0.01 | +0.04 | +0.03 | −0.01 | 0.05 | 0.07 |
| 18120653−3654264 | +0.00 | +0.03 | +0.03 | −0.01 | 0.05 | 0.07 |
| 18110179−3630394 | +0.00 | +0.04 | +0.04 | −0.01 | 0.05 | 0.08 |
| 18124892−3626403 | −0.01 | +0.04 | +0.03 | −0.01 | 0.05 | 0.07 |
| 18135164−3643463 | −0.01 | +0.04 | +0.04 | −0.01 | 0.02 | 0.06 |
| 18124339−3635339 | −0.01 | +0.05 | +0.04 | −0.02 | 0.05 | 0.08 |
| 18113921−3652069 | −0.04 | +0.07 | +0.05 | −0.02 | 0.05 | 0.11 |
| 18111325−3646007 | −0.01 | +0.05 | +0.05 | −0.02 | 0.15 | 0.17 |
| 18113833−3626322 | −0.05 | +0.07 | +0.07 | −0.03 | 0.05 | 0.13 |
| 18111018−3639350 | −0.05 | +0.07 | +0.06 | −0.02 | 0.05 | 0.12 |
| 18135243−3630481 | −0.02 | +0.04 | +0.05 | −0.02 | 0.05 | 0.09 |
| 18121150−3627559 | −0.04 | +0.06 | +0.06 | −0.02 | 0.05 | 0.11 |
| 18111963−3647245 | −0.05 | +0.08 | +0.06 | −0.03 | 0.03 | 0.12 |
| 18140023−3635461 | −0.06 | +0.09 | +0.07 | −0.05 | 0.02 | 0.14 |
| 18135881−3639345 | −0.05 | +0.09 | +0.06 | −0.02 | 0.05 | 0.13 |
| 18121436−3654551 | −0.07 | +0.10 | +0.07 | −0.05 | 0.05 | 0.16 |
| 18124228−3655079 | −0.07 | +0.08 | +0.07 | −0.04 | 0.05 | 0.14 |
| 18122530−3637366 | −0.06 | +0.11 | +0.06 | −0.04 | 0.13 | 0.19 |
| 18131370−3651584 | −0.06 | +0.08 | +0.05 | −0.04 | 0.05 | 0.13 |
| 18134668−3623541 | ... | ... | ... | ... | ... | ... |
| 18105081−3642137 | −0.03 | +0.05 | +0.05 | −0.03 | 0.05 | 0.10 |
| 18124219−3631172 | −0.07 | +0.09 | +0.06 | −0.04 | 0.00 | 0.13 |
| 18133688−3647054 | ... | ... | ... | ... | ... | ... |
| 18123142−3639294 | −0.08 | +0.11 | +0.04 | −0.03 | 0.05 | 0.15 |
| 18133038−3632229 | −0.03 | +0.06 | +0.04 | −0.03 | 0.05 | 0.10 |
| 18133292−3624179 | ... | ... | ... | ... | ... | ... |
| 18111681−3636318 | −0.09 | +0.06 | +0.04 | −0.03 | 0.05 | 0.13 |
| 18105004−3640063 | −0.04 | +0.05 | +0.05 | −0.03 | 0.05 | 0.10 |
| 18112334−3634194 | −0.05 | +0.06 | +0.06 | −0.03 | 0.08 | 0.13 |
| 18131027−3632343 | −0.07 | +0.08 | +0.05 | −0.04 | 0.04 | 0.13 |
| 18110293−3628041 | −0.09 | +0.08 | +0.05 | −0.05 | 0.11 | 0.18 |
| 18132040−3623075 | −0.07 | +0.05 | +0.06 | −0.03 | 0.07 | 0.13 |
| 18135588−3629188 | −0.05 | +0.06 | +0.06 | −0.03 | 0.03 | 0.11 |
| 18105075−3635061 | −0.09 | +0.10 | +0.06 | −0.04 | 0.11 | 0.19 |
| 18104188−3634541 | −0.03 | +0.07 | +0.05 | −0.03 | 0.05 | 0.11 |
| 18132998−3628578 | −0.09 | +0.10 | +0.06 | −0.03 | 0.00 | 0.15 |
| 18130544−3616563 | −0.08 | +0.10 | +0.06 | −0.05 | 0.05 | 0.16 |
| 18115908−3654510 | −0.08 | +0.12 | +0.07 | −0.05 | 0.05 | 0.18 |
| 18121077−3639094 | −0.08 | +0.07 | +0.07 | −0.04 | 0.05 | 0.14 |
| 18120614−3629571 | −0.06 | +0.05 | +0.07 | −0.04 | 0.05 | 0.12 |
| 18120213−3641599 | −0.04 | +0.07 | +0.07 | −0.05 | 0.05 | 0.13 |
| 18123350−3654398 | −0.10 | +0.10 | +0.08 | −0.06 | 0.09 | 0.20 |
| 18120973−3654184 | −0.11 | +0.10 | +0.09 | −0.06 | 0.05 | 0.19 |
| 18105641−3632359 | −0.08 | +0.04 | +0.08 | −0.05 | 0.05 | 0.14 |
| 18125106−3654091 | −0.04 | +0.07 | +0.07 | −0.04 | 0.10 | 0.15 |
| 18111581−3648469 | −0.10 | +0.10 | +0.09 | −0.04 | 0.11 | 0.20 |
| 18131387−3630130 | −0.07 | +0.10 | +0.08 | −0.04 | 0.05 | 0.16 |
| 18123592−3634476 | −0.09 | +0.11 | +0.09 | −0.03 | 0.05 | 0.18 |
| 18135736−3638266 | −0.08 | +0.08 | +0.08 | −0.04 | 0.05 | 0.15 |
| 18133233−3626133 | −0.09 | +0.11 | +0.09 | −0.03 | 0.07 | 0.18 |
| 18125003−3630269 | −0.07 | +0.05 | +0.08 | −0.05 | 0.05 | 0.14 |
| 18130723−3618385 | −0.05 | +0.06 | +0.07 | −0.05 | 0.11 | 0.16 |
| 18125800−3616427 | −0.03 | +0.07 | +0.06 | −0.03 | 0.05 | 0.11 |
| 18111323−3637030 | −0.05 | +0.07 | +0.06 | −0.04 | 0.15 | 0.19 |
| 18130427−3630012 | −0.04 | +0.08 | +0.06 | −0.05 | 0.05 | 0.13 |
| 18124614−3617326 | −0.09 | +0.08 | +0.07 | −0.05 | 0.02 | 0.15 |
| 18120399−3615387 | −0.08 | +0.09 | +0.07 | −0.03 | 0.09 | 0.17 |
| 18123475−3624478 | −0.06 | +0.08 | +0.07 | −0.04 | 0.05 | 0.14 |
| 18115661−3617533 | −0.05 | +0.08 | +0.05 | −0.05 | 0.09 | 0.15 |
| 18113299−3623341 | −0.09 | +0.07 | +0.06 | −0.05 | 0.03 | 0.14 |
| 18111553−3628156 | −0.09 | +0.09 | +0.05 | −0.04 | 0.03 | 0.15 |
| 18125907−3644275 | −0.04 | +0.08 | +0.05 | −0.04 | 0.05 | 0.12 |
| 18111726−3620302 | ... | ... | ... | ... | ... | ... |
| 18111579−3625114 | −0.10 | +0.11 | +0.03 | −0.04 | 0.00 | 0.16 |
| 18131305−3650449 | −0.06 | +0.09 | +0.04 | −0.05 | 0.06 | 0.14 |
| 18123152−3636498 | −0.11 | +0.09 | +0.03 | −0.05 | 0.08 | 0.17 |
| 18125914−3619208 | −0.06 | +0.09 | +0.04 | −0.05 | 0.01 | 0.13 |
| 18115073−3650493 | −0.08 | +0.07 | +0.03 | −0.05 | 0.04 | 0.13 |
| 18114648−3625169 | −0.04 | +0.07 | +0.04 | −0.06 | 0.09 | 0.14 |
| 18113751−3629139 | −0.11 | +0.09 | +0.02 | −0.05 | 0.02 | 0.15 |
| 18122243−3637539 | −0.08 | +0.08 | +0.04 | −0.04 | 0.07 | 0.14 |
| 18133366−3644575 | −0.04 | +0.08 | +0.05 | −0.05 | 0.03 | 0.12 |
| 18134702−3641477 | −0.05 | +0.08 | +0.05 | −0.06 | 0.03 | 0.13 |
| 18125228−3618294 | −0.05 | +0.09 | +0.05 | −0.05 | 0.05 | 0.13 |
| 18110942−3647198 | −0.04 | +0.09 | +0.05 | −0.04 | 0.05 | 0.13 |
| 18104824−3638507 | −0.10 | +0.10 | +0.03 | −0.04 | 0.05 | 0.16 |
| 18122301−3629462 | −0.10 | +0.10 | +0.03 | −0.04 | 0.02 | 0.15 |
| 18133332−3645578 | −0.11 | +0.10 | +0.03 | −0.05 | 0.13 | 0.21 |
| 18123434−3652241 | −0.08 | +0.07 | +0.04 | −0.05 | 0.01 | 0.12 |
| 18112311−3625456 | −0.06 | +0.10 | +0.05 | −0.04 | 0.05 | 0.14 |
| 18125463−3649277 | −0.08 | +0.07 | +0.05 | −0.04 | 0.05 | 0.13 |
| 18123925−3620465 | −0.10 | +0.08 | +0.04 | −0.04 | 0.02 | 0.14 |
| 18110629−3632146 | −0.09 | +0.05 | +0.04 | −0.04 | 0.02 | 0.12 |
| 18133687−3639590 | −0.05 | +0.10 | +0.05 | −0.05 | 0.04 | 0.14 |
| 18111505−3620576 | −0.05 | +0.10 | +0.05 | −0.05 | 0.03 | 0.14 |
| 18120832−3628243 | −0.09 | +0.06 | +0.05 | −0.06 | 0.00 | 0.13 |
| 18130815−3631460 | −0.11 | +0.12 | +0.04 | −0.05 | 0.13 | 0.22 |
| 18120407−3636481 | −0.09 | +0.08 | +0.04 | −0.04 | 0.02 | 0.13 |
| 18135786−3640300 | −0.08 | +0.11 | +0.05 | −0.05 | 0.05 | 0.16 |
| 18131228−3619138 | −0.08 | +0.08 | +0.06 | −0.05 | 0.12 | 0.18 |
| 18113372−3650200 | ... | ... | ... | ... | ... | ... |
| 18115904−3650428 | −0.10 | +0.07 | +0.07 | −0.05 | 0.06 | 0.16 |
| 18115448−3641161 | −0.07 | +0.09 | +0.07 | −0.05 | 0.14 | 0.20 |
| 18123678−3649019 | −0.05 | +0.09 | +0.08 | −0.04 | 0.10 | 0.17 |
| 18113965−3645408 | −0.08 | +0.09 | +0.07 | −0.03 | 0.20 | 0.25 |
| 18135362−3636538 | −0.06 | +0.12 | +0.07 | −0.04 | 0.17 | 0.23 |
| 18123168−3631555 | −0.04 | +0.09 | +0.07 | −0.04 | 0.05 | 0.14 |
| 18115398−3623290 | −0.09 | +0.07 | +0.07 | −0.03 | 0.05 | 0.15 |
| 18123393−3615508 | −0.05 | +0.09 | +0.07 | −0.05 | 0.04 | 0.14 |
| 18120689−3643231 | −0.05 | +0.11 | +0.07 | −0.05 | 0.10 | 0.18 |
| 18130482−3649019 | −0.10 | +0.06 | +0.06 | −0.03 | 0.20 | 0.24 |
| 18110352−3646275 | −0.10 | +0.10 | +0.06 | −0.05 | 0.08 | 0.18 |
| 18105013−3629557 | −0.08 | +0.10 | +0.06 | −0.05 | 0.10 | 0.18 |
| 18121897−3630243 | −0.05 | +0.09 | +0.06 | −0.07 | 0.00 | 0.14 |
| 18122029−3652333 | −0.07 | +0.11 | +0.06 | −0.05 | 0.13 | 0.20 |
| (l, b) = (+8.5, +9) | ||||||
| 17311256−1702018 | −0.04 | +0.07 | +0.05 | −0.02 | 0.00 | 0.10 |
| 17290874−1632431 | −0.07 | +0.09 | +0.05 | −0.02 | 0.05 | 0.14 |
| 17302885−1639588 | −0.06 | +0.06 | +0.06 | −0.02 | 0.05 | 0.12 |
| 17304789−1623192 | −0.05 | +0.05 | +0.07 | −0.02 | 0.02 | 0.10 |
| 17321080−1641479 | −0.08 | +0.09 | +0.08 | −0.02 | 0.05 | 0.15 |
| 17303589−1638299 | −0.07 | +0.06 | +0.08 | −0.03 | 0.05 | 0.14 |
| 17290513−1630383 | −0.09 | +0.08 | +0.08 | −0.03 | 0.01 | 0.15 |
| 17314699−1654460 | −0.06 | +0.08 | +0.07 | −0.02 | 0.01 | 0.12 |
| 17305076−1615216 | −0.08 | +0.07 | +0.05 | −0.04 | 0.05 | 0.13 |
| 17323324−1627474 | −0.11 | +0.11 | +0.03 | −0.04 | 0.10 | 0.19 |
| 17312795−1631423 | −0.07 | +0.10 | +0.05 | −0.03 | 0.03 | 0.14 |
| 17290285−1638344 | −0.07 | +0.12 | +0.05 | −0.03 | 0.02 | 0.15 |
| 17303378−1703086 | −0.10 | +0.11 | +0.05 | −0.04 | 0.02 | 0.16 |
| 17304223−1609274 | −0.10 | +0.09 | +0.07 | −0.04 | 0.05 | 0.16 |
| 17304908−1633101 | −0.10 | +0.09 | +0.06 | −0.03 | 0.02 | 0.15 |
| 17291459−1650085 | −0.10 | +0.08 | +0.07 | −0.03 | 0.05 | 0.16 |
| 17300674−1638541 | −0.11 | +0.08 | +0.07 | −0.04 | 0.06 | 0.17 |
| 17315010−1653413 | −0.08 | +0.08 | +0.08 | −0.04 | 0.24 | 0.28 |
| 17295493−1613273 | −0.11 | +0.06 | +0.08 | −0.06 | 0.05 | 0.17 |
| 17311523−1618542 | −0.08 | +0.08 | +0.09 | −0.05 | 0.09 | 0.18 |
| 17314811−1621558 | −0.09 | +0.11 | +0.08 | −0.04 | 0.09 | 0.19 |
| 17304861−1646459 | −0.11 | +0.07 | +0.09 | −0.03 | 0.05 | 0.17 |
| 17323959−1625298 | −0.09 | +0.10 | +0.09 | −0.05 | 0.03 | 0.17 |
| 17285711−1633566 | −0.09 | +0.12 | +0.09 | −0.04 | 0.05 | 0.19 |
| 17314673−1641228 | −0.10 | +0.07 | +0.08 | −0.03 | 0.00 | 0.15 |
| 17294476−1626118 | −0.11 | +0.08 | +0.07 | −0.03 | 0.04 | 0.16 |
| 17320650−1643389 | −0.11 | +0.07 | +0.04 | −0.03 | 0.02 | 0.14 |
| 17314427−1640265 | −0.09 | +0.07 | +0.06 | −0.04 | 0.01 | 0.14 |
| 17300064−1701075 | −0.11 | +0.07 | +0.04 | −0.03 | 0.05 | 0.15 |
| 17302935−1652277 | −0.09 | +0.09 | +0.04 | −0.04 | 0.18 | 0.23 |
| 17320652−1619563 | −0.11 | +0.14 | +0.01 | −0.05 | 0.05 | 0.19 |
| 17304464−1631471 | −0.10 | +0.10 | +0.03 | −0.04 | 0.02 | 0.15 |
| 17321715−1632467 | −0.10 | +0.11 | +0.02 | −0.05 | 0.13 | 0.20 |
| 17321969−1653156 | −0.10 | +0.13 | +0.02 | −0.03 | 0.02 | 0.17 |
| 17315690−1630315 | −0.11 | +0.12 | +0.02 | −0.05 | 0.05 | 0.18 |
| 17312870−1619572 | −0.11 | +0.12 | +0.02 | −0.04 | 0.20 | 0.26 |
| 17294541−1649018 | −0.11 | +0.12 | +0.02 | −0.03 | 0.13 | 0.21 |
| 17305067−1644006 | −0.11 | +0.13 | +0.02 | −0.03 | 0.11 | 0.21 |
| 17312457−1652524 | −0.10 | +0.08 | +0.04 | −0.05 | 0.04 | 0.15 |
| 17292760−1636235 | −0.09 | +0.11 | +0.04 | −0.02 | 0.16 | 0.22 |
| 17295978−1633590 | −0.11 | +0.15 | +0.02 | −0.04 | 0.08 | 0.21 |
| 17322323−1649335 | −0.10 | +0.08 | +0.03 | −0.04 | 0.00 | 0.14 |
| 17321117−1654590 | −0.10 | +0.08 | +0.03 | −0.04 | 0.04 | 0.14 |
| 17313606−1607539 | −0.09 | +0.08 | +0.04 | −0.05 | 0.02 | 0.14 |
| 17295331−1653069 | −0.10 | +0.08 | +0.04 | −0.04 | 0.05 | 0.15 |
| 17302818−1636032 | −0.09 | +0.10 | +0.05 | −0.04 | 0.04 | 0.15 |
| 17293118−1638081 | −0.09 | +0.06 | +0.05 | −0.04 | 0.28 | 0.31 |
| 17291994−1618302 | −0.11 | +0.14 | +0.04 | −0.03 | 0.09 | 0.21 |
| 17320457−1646391 | −0.10 | +0.10 | +0.05 | −0.04 | 0.06 | 0.17 |
| 17310747−1620049 | −0.09 | +0.08 | +0.06 | −0.04 | 0.11 | 0.18 |
| 17323392−1636330 | ... | ... | ... | ... | ... | ... |
| 17312572−1609092 | −0.09 | +0.07 | +0.06 | −0.05 | 0.02 | 0.14 |
| 17300015−1609464 | −0.09 | +0.08 | +0.07 | −0.04 | 0.05 | 0.15 |
| 17305894−1637056 | −0.10 | +0.16 | +0.06 | −0.03 | 0.05 | 0.21 |
| 17291621−1647189 | −0.10 | +0.16 | +0.06 | −0.04 | 0.05 | 0.21 |
| 17302194−1643531 | −0.09 | +0.14 | +0.06 | −0.02 | 0.15 | 0.23 |
| 17311959−1643577 | −0.09 | +0.09 | +0.06 | −0.03 | 0.00 | 0.14 |
| 17311229−1659047 | −0.10 | +0.13 | +0.02 | −0.03 | 0.05 | 0.18 |
| 17313313−1659216 | −0.09 | +0.10 | +0.04 | −0.04 | 0.12 | 0.19 |
| 17301749−1629529 | −0.10 | +0.06 | +0.05 | −0.04 | 0.13 | 0.19 |
| 17294261−1622440 | −0.10 | +0.09 | +0.04 | −0.03 | 0.05 | 0.15 |
| 17323625−1637551 | −0.09 | +0.09 | +0.06 | −0.04 | 0.04 | 0.15 |
| 17314292−1620036 | −0.10 | +0.11 | +0.06 | −0.03 | 0.01 | 0.16 |
| 17310955−1635152 | −0.11 | +0.13 | +0.07 | −0.05 | 0.05 | 0.20 |
| 17304312−1630318 | −0.09 | +0.08 | +0.06 | −0.04 | 0.05 | 0.15 |
| 17285469−1627232 | −0.09 | +0.13 | +0.06 | −0.04 | 0.10 | 0.20 |
| 17310360−1700146 | −0.10 | +0.07 | +0.06 | −0.05 | 0.05 | 0.15 |
| 17295898−1652101 | −0.09 | +0.10 | +0.06 | −0.04 | 0.05 | 0.16 |
Table 8. Abundance Uncertainty: Calcium
| Star ID | ΔTeff | Δlog(g) | Δ[M/H] | ΔVt | σ/√(N) | ΔTotal |
|---|---|---|---|---|---|---|
| 2MASS | (+100 K) | (+0.3 cgs) | (+0.3 dex) | (+0.3 km s-1) | ||
| (l, b) = (−5.5, −7) | ||||||
| 18011989−3723462 | +0.09 | −0.02 | −0.03 | −0.07 | 0.06 | 0.13 |
| 18003452−3729217 | +0.09 | −0.01 | −0.02 | −0.05 | 0.10 | 0.15 |
| 18011692−3722508 | +0.11 | −0.01 | −0.02 | −0.09 | 0.06 | 0.16 |
| 18005584−3739103 | ... | ... | ... | ... | ... | ... |
| 18015010−3735279 | +0.10 | −0.01 | −0.02 | −0.11 | 0.04 | 0.16 |
| 18005916−3727585 | +0.11 | −0.02 | −0.02 | −0.12 | 0.03 | 0.17 |
| 18005027−3707505 | +0.09 | −0.01 | −0.02 | −0.07 | 0.03 | 0.12 |
| 18005234−3715478 | +0.10 | −0.01 | −0.02 | −0.14 | 0.06 | 0.18 |
| 18020106−3737561 | +0.11 | −0.01 | −0.02 | −0.14 | 0.05 | 0.19 |
| 17595541−3713447 | ... | ... | ... | ... | ... | ... |
| 17595664−3725304 | +0.09 | −0.02 | −0.02 | −0.12 | 0.00 | 0.15 |
| 18021345−3730371 | +0.12 | −0.01 | −0.02 | −0.15 | 0.04 | 0.20 |
| 17594241−3718247 | ... | ... | ... | ... | ... | ... |
| 18013342−3726339 | +0.10 | −0.02 | −0.02 | −0.12 | 0.04 | 0.16 |
| 18003204−3726008 | +0.11 | −0.02 | +0.00 | −0.17 | 0.07 | 0.22 |
| 18013580−3740055 | +0.12 | −0.01 | −0.01 | −0.15 | 0.06 | 0.20 |
| 18013799−3725131 | +0.12 | −0.02 | +0.00 | −0.16 | 0.04 | 0.20 |
| 18022149−3713494 | +0.11 | −0.01 | −0.01 | −0.14 | 0.02 | 0.18 |
| 18011408−3711299 | +0.09 | −0.01 | −0.02 | −0.13 | 0.07 | 0.17 |
| 18021275−3737543 | +0.10 | −0.02 | −0.01 | −0.15 | 0.01 | 0.18 |
| 17595027−3727293 | +0.11 | −0.02 | −0.01 | −0.15 | 0.06 | 0.20 |
| 18002115−3715519 | +0.11 | −0.02 | +0.02 | −0.17 | 0.07 | 0.22 |
| 17595366−3728186 | +0.09 | −0.01 | −0.02 | −0.14 | 0.02 | 0.17 |
| 18001354−3709122 | +0.11 | −0.01 | +0.02 | −0.17 | 0.02 | 0.20 |
| 18013960−3723398 | +0.10 | −0.02 | +0.02 | −0.17 | 0.03 | 0.20 |
| 18021862−3734204 | +0.11 | −0.01 | +0.01 | −0.16 | 0.05 | 0.20 |
| 18000535−3735315 | +0.11 | −0.01 | +0.01 | −0.17 | 0.01 | 0.20 |
| 18013848−3721442 | +0.11 | −0.01 | +0.01 | −0.16 | 0.05 | 0.20 |
| 17594792−3721422 | +0.11 | −0.03 | +0.00 | −0.16 | 0.02 | 0.20 |
| 18011941−3721250 | +0.11 | +0.00 | +0.02 | −0.16 | 0.02 | 0.20 |
| 18004824−3718074 | +0.10 | −0.02 | +0.03 | −0.18 | 0.03 | 0.21 |
| 18014343−3708232 | +0.11 | −0.01 | +0.02 | −0.17 | 0.11 | 0.23 |
| 18005852−3711524 | +0.09 | −0.03 | −0.01 | −0.16 | 0.08 | 0.20 |
| 18020816−3714015 | +0.10 | −0.01 | −0.01 | −0.15 | 0.05 | 0.19 |
| 18010932−3702079 | +0.10 | −0.01 | +0.03 | −0.17 | 0.03 | 0.20 |
| 18010065−3740456 | +0.10 | −0.01 | +0.03 | −0.18 | 0.05 | 0.21 |
| 17595640−3710383 | +0.11 | −0.03 | +0.00 | −0.17 | 0.00 | 0.20 |
| 18012462−3738382 | +0.10 | −0.01 | −0.01 | −0.15 | 0.06 | 0.19 |
| 18002880−3710171 | +0.09 | −0.01 | −0.02 | −0.15 | 0.05 | 0.18 |
| 18024484−3714159 | +0.09 | −0.01 | −0.01 | −0.15 | 0.07 | 0.19 |
| 18013206−3708133 | ... | ... | ... | ... | ... | ... |
| 18004074−3740058 | +0.11 | −0.02 | −0.01 | −0.16 | 0.05 | 0.20 |
| 18000013−3715053 | +0.11 | −0.02 | +0.00 | −0.16 | 0.08 | 0.21 |
| 18015431−3717070 | +0.10 | −0.01 | −0.01 | −0.16 | 0.05 | 0.20 |
| 18021006−3738193 | +0.08 | −0.02 | −0.02 | −0.16 | 0.05 | 0.19 |
| 17595442−3721118 | +0.11 | −0.01 | +0.00 | −0.17 | 0.03 | 0.20 |
| 18021721−3736096 | +0.09 | +0.00 | −0.02 | −0.14 | 0.09 | 0.19 |
| 18005096−3733499 | ... | ... | ... | ... | ... | ... |
| 18005923−3707111 | +0.09 | −0.02 | +0.01 | −0.18 | 0.02 | 0.20 |
| 18011851−3706092 | +0.10 | −0.02 | +0.01 | −0.18 | 0.05 | 0.21 |
| 18013395−3705551 | +0.09 | −0.03 | +0.03 | −0.18 | 0.08 | 0.22 |
| 18022648−3728188 | +0.09 | +0.00 | −0.02 | −0.15 | 0.04 | 0.18 |
| 18024919−3727234 | +0.09 | +0.00 | −0.01 | −0.15 | 0.06 | 0.19 |
| 18023660−3716289 | +0.09 | +0.00 | −0.01 | −0.14 | 0.08 | 0.18 |
| 17595509−3711099 | +0.10 | −0.01 | +0.00 | −0.17 | 0.05 | 0.20 |
| 18005395−3731231 | +0.08 | −0.01 | +0.02 | −0.18 | 0.09 | 0.22 |
| 18010322−3705447 | +0.08 | +0.00 | −0.01 | −0.15 | 0.03 | 0.17 |
| 18014769−3739220 | ... | ... | ... | ... | ... | ... |
| 17594807−3715283 | +0.09 | −0.02 | +0.00 | −0.17 | 0.04 | 0.20 |
| 18013618−3706311 | +0.10 | −0.02 | +0.02 | −0.18 | 0.03 | 0.21 |
| 18004314−3730156 | +0.09 | −0.01 | +0.00 | −0.17 | 0.03 | 0.19 |
| 18014303−3740054 | +0.10 | −0.02 | +0.02 | −0.18 | 0.06 | 0.22 |
| 18003751−3728200 | +0.08 | −0.01 | +0.04 | −0.20 | 0.07 | 0.23 |
| 18011170−3727118 | +0.09 | +0.00 | +0.00 | −0.12 | 0.02 | 0.15 |
| 18023846−3718345 | +0.10 | −0.02 | +0.03 | −0.18 | 0.05 | 0.21 |
| 18011671−3722213 | ... | ... | ... | ... | ... | ... |
| 18005985−3734507 | ... | ... | ... | ... | ... | ... |
| 18000430−3711051 | +0.10 | −0.02 | +0.04 | −0.19 | 0.01 | 0.22 |
| 18003552−3729476 | +0.10 | −0.01 | +0.03 | −0.18 | 0.07 | 0.22 |
| 18001817−3732243 | +0.09 | −0.02 | +0.02 | −0.19 | 0.09 | 0.23 |
| 18013039−3713086 | +0.09 | −0.01 | +0.03 | −0.17 | 0.01 | 0.20 |
| 18012564−3741052 | +0.10 | −0.01 | +0.03 | −0.18 | 0.05 | 0.21 |
| 18025713−3718318 | +0.08 | −0.01 | +0.04 | −0.20 | 0.09 | 0.24 |
| 18011599−3741385 | +0.09 | −0.02 | +0.03 | −0.19 | 0.05 | 0.22 |
| 18012944−3719488 | +0.09 | +0.00 | +0.00 | −0.15 | 0.06 | 0.18 |
| 18020361−3719086 | +0.09 | +0.00 | +0.01 | −0.17 | 0.10 | 0.22 |
| 18024024−3728187 | +0.08 | −0.01 | +0.04 | −0.18 | 0.10 | 0.22 |
| 18000412−3717266 | +0.07 | −0.02 | +0.05 | −0.19 | 0.03 | 0.21 |
| 18011177−3703344 | +0.09 | −0.02 | +0.05 | −0.19 | 0.09 | 0.23 |
| 18001410−3725181 | +0.07 | −0.02 | +0.06 | −0.20 | 0.06 | 0.23 |
| 18020300−3719418 | +0.07 | −0.03 | +0.05 | −0.20 | 0.05 | 0.23 |
| 18004683−3703252 | +0.07 | −0.02 | +0.05 | −0.19 | 0.04 | 0.21 |
| 18015404−3722564 | +0.10 | −0.02 | +0.03 | −0.19 | 0.03 | 0.22 |
| 18013974−3704068 | +0.09 | −0.01 | +0.03 | −0.19 | 0.04 | 0.22 |
| 18020704−3708064 | +0.09 | +0.00 | +0.00 | −0.19 | 0.00 | 0.21 |
| 18023393−3730273 | ... | ... | ... | ... | ... | ... |
| 18001720−3708374 | +0.06 | −0.02 | +0.06 | −0.20 | 0.04 | 0.22 |
| 18003663−3708547 | +0.08 | −0.02 | +0.04 | −0.20 | 0.04 | 0.22 |
| 18002569−3729578 | +0.09 | −0.01 | +0.02 | −0.20 | 0.09 | 0.24 |
| 17594881−3716203 | +0.09 | −0.03 | +0.06 | −0.19 | 0.03 | 0.22 |
| 18011201−3740090 | +0.09 | +0.00 | +0.02 | −0.19 | 0.05 | 0.22 |
| (l, b) = (−4, −9) | ||||||
| 18122552−3653049 | +0.10 | −0.02 | −0.02 | −0.08 | 0.05 | 0.14 |
| 18120653−3654264 | +0.08 | −0.02 | −0.02 | −0.08 | 0.04 | 0.12 |
| 18110179−3630394 | +0.10 | −0.02 | −0.02 | −0.08 | 0.05 | 0.14 |
| 18124892−3626403 | +0.08 | −0.02 | −0.02 | −0.08 | 0.03 | 0.12 |
| 18135164−3643463 | +0.10 | −0.02 | −0.02 | −0.07 | 0.06 | 0.14 |
| 18124339−3635339 | +0.11 | −0.02 | −0.02 | −0.10 | 0.11 | 0.19 |
| 18113921−3652069 | +0.10 | −0.01 | −0.02 | −0.08 | 0.05 | 0.14 |
| 18111325−3646007 | +0.11 | −0.02 | −0.02 | −0.12 | 0.00 | 0.17 |
| 18113833−3626322 | +0.12 | −0.01 | −0.02 | −0.12 | 0.06 | 0.18 |
| 18111018−3639350 | +0.11 | −0.02 | −0.02 | −0.12 | 0.06 | 0.18 |
| 18135243−3630481 | +0.10 | −0.02 | −0.02 | −0.09 | 0.06 | 0.15 |
| 18121150−3627559 | +0.10 | −0.01 | −0.02 | −0.10 | 0.04 | 0.15 |
| 18111963−3647245 | +0.11 | −0.01 | −0.02 | −0.14 | 0.02 | 0.18 |
| 18140023−3635461 | +0.10 | +0.00 | −0.02 | −0.11 | 0.05 | 0.16 |
| 18135881−3639345 | +0.11 | −0.01 | −0.02 | −0.13 | 0.05 | 0.18 |
| 18121436−3654551 | +0.12 | −0.01 | −0.02 | −0.14 | 0.04 | 0.19 |
| 18124228−3655079 | +0.12 | −0.01 | −0.01 | −0.13 | 0.04 | 0.18 |
| 18122530−3637366 | +0.12 | −0.01 | −0.02 | −0.14 | 0.00 | 0.19 |
| 18131370−3651584 | +0.10 | −0.01 | −0.02 | −0.15 | 0.04 | 0.19 |
| 18134668−3623541 | +0.11 | −0.01 | −0.02 | −0.12 | 0.03 | 0.17 |
| 18105081−3642137 | +0.09 | −0.03 | −0.02 | −0.15 | 0.00 | 0.18 |
| 18124219−3631172 | +0.11 | −0.01 | −0.02 | −0.14 | 0.03 | 0.18 |
| 18133688−3647054 | ... | ... | ... | ... | ... | ... |
| 18123142−3639294 | +0.12 | −0.01 | −0.01 | −0.16 | 0.01 | 0.20 |
| 18133038−3632229 | ... | ... | ... | ... | ... | |
| 18133292−3624179 | ... | ... | ... | ... | ... | |
| 18111681−3636318 | +0.11 | −0.02 | −0.01 | −0.16 | 0.02 | 0.20 |
| 18105004−3640063 | ... | ... | ... | ... | ... | |
| 18112334−3634194 | +0.10 | −0.03 | −0.02 | −0.15 | 0.05 | 0.19 |
| 18131027−3632343 | +0.11 | −0.02 | −0.02 | −0.15 | 0.00 | 0.19 |
| 18110293−3628041 | +0.12 | −0.01 | −0.01 | −0.15 | 0.06 | 0.20 |
| 18132040−3623075 | +0.11 | −0.03 | −0.01 | −0.15 | 0.05 | 0.20 |
| 18135588−3629188 | +0.10 | −0.01 | −0.02 | −0.12 | 0.06 | 0.17 |
| 18105075−3635061 | +0.11 | −0.02 | +0.00 | −0.17 | 0.03 | 0.21 |
| 18104188−3634541 | +0.09 | +0.00 | −0.02 | −0.11 | 0.06 | 0.16 |
| 18132998−3628578 | +0.11 | −0.01 | +0.00 | −0.15 | 0.03 | 0.19 |
| 18130544−3616563 | +0.12 | −0.02 | +0.00 | −0.16 | 0.03 | 0.20 |
| 18115908−3654510 | +0.11 | −0.01 | +0.00 | −0.17 | 0.04 | 0.21 |
| 18121077−3639094 | +0.11 | −0.02 | −0.01 | −0.14 | 0.03 | 0.18 |
| 18120614−3629571 | +0.10 | −0.02 | −0.01 | −0.15 | 0.03 | 0.18 |
| 18120213−3641599 | +0.09 | −0.01 | −0.02 | −0.14 | 0.01 | 0.17 |
| 18123350−3654398 | +0.10 | −0.02 | +0.02 | −0.17 | 0.07 | 0.21 |
| 18120973−3654184 | +0.10 | −0.01 | +0.03 | −0.16 | 0.04 | 0.20 |
| 18105641−3632359 | +0.11 | −0.03 | +0.00 | −0.16 | 0.04 | 0.20 |
| 18125106−3654091 | +0.09 | −0.01 | −0.01 | −0.15 | 0.05 | 0.18 |
| 18111581−3648469 | +0.10 | −0.02 | +0.03 | −0.18 | 0.03 | 0.21 |
| 18131387−3630130 | +0.12 | −0.01 | +0.01 | −0.16 | 0.01 | 0.20 |
| 18123592−3634476 | +0.10 | −0.01 | +0.03 | −0.16 | 0.05 | 0.20 |
| 18135736−3638266 | +0.11 | −0.03 | +0.02 | −0.17 | 0.01 | 0.21 |
| 18133233−3626133 | +0.10 | −0.01 | +0.03 | −0.17 | 0.05 | 0.21 |
| 18125003−3630269 | +0.10 | −0.02 | −0.01 | −0.14 | 0.05 | 0.18 |
| 18130723−3618385 | +0.10 | −0.02 | −0.01 | −0.16 | 0.05 | 0.20 |
| 18125800−3616427 | +0.09 | −0.02 | −0.01 | −0.15 | 0.06 | 0.19 |
| 18111323−3637030 | +0.09 | −0.02 | −0.01 | −0.16 | 0.07 | 0.20 |
| 18130427−3630012 | +0.08 | −0.01 | −0.02 | −0.14 | 0.09 | 0.19 |
| 18124614−3617326 | +0.11 | −0.01 | +0.00 | −0.16 | 0.07 | 0.21 |
| 18120399−3615387 | +0.11 | −0.02 | +0.02 | −0.17 | 0.08 | 0.22 |
| 18123475−3624478 | +0.10 | −0.02 | −0.01 | −0.15 | 0.00 | 0.18 |
| 18115661−3617533 | +0.09 | −0.02 | −0.02 | −0.16 | 0.05 | 0.19 |
| 18113299−3623341 | +0.11 | −0.03 | +0.01 | −0.18 | 0.05 | 0.22 |
| 18111553−3628156 | +0.11 | −0.02 | +0.02 | −0.17 | 0.02 | 0.21 |
| 18125907−3644275 | +0.09 | +0.00 | −0.02 | −0.12 | 0.06 | 0.16 |
| 18111726−3620302 | +0.11 | −0.01 | −0.01 | −0.15 | 0.02 | 0.19 |
| 18111579−3625114 | +0.09 | −0.04 | +0.04 | −0.18 | 0.03 | 0.21 |
| 18131305−3650449 | +0.09 | −0.02 | −0.02 | −0.16 | 0.01 | 0.19 |
| 18123152−3636498 | +0.09 | −0.03 | +0.03 | −0.18 | 0.05 | 0.21 |
| 18125914−3619208 | +0.09 | −0.01 | −0.02 | −0.17 | 0.02 | 0.19 |
| 18115073−3650493 | +0.10 | −0.01 | −0.02 | −0.15 | 0.05 | 0.19 |
| 18114648−3625169 | +0.08 | −0.01 | −0.02 | −0.15 | 0.06 | 0.18 |
| 18113751−3629139 | +0.09 | −0.03 | +0.03 | −0.18 | 0.07 | 0.22 |
| 18122243−3637539 | +0.10 | −0.02 | +0.00 | −0.17 | 0.06 | 0.21 |
| 18133366−3644575 | ... | ... | ... | ... | ... | |
| 18134702−3641477 | +0.08 | −0.01 | −0.02 | −0.16 | 0.03 | 0.18 |
| 18125228−3618294 | +0.09 | −0.01 | −0.02 | −0.17 | 0.07 | 0.21 |
| 18110942−3647198 | +0.08 | +0.00 | −0.01 | −0.13 | 0.09 | 0.18 |
| 18104824−3638507 | +0.09 | −0.02 | +0.03 | −0.19 | 0.05 | 0.22 |
| 18122301−3629462 | +0.08 | −0.01 | +0.03 | −0.18 | 0.03 | 0.20 |
| 18133332−3645578 | +0.08 | −0.02 | +0.03 | −0.18 | 0.02 | 0.20 |
| 18123434−3652241 | +0.10 | −0.02 | +0.00 | −0.17 | 0.05 | 0.20 |
| 18112311−3625456 | +0.09 | −0.01 | −0.01 | −0.16 | 0.03 | 0.19 |
| 18125463−3649277 | +0.10 | −0.02 | +0.00 | −0.17 | 0.06 | 0.21 |
| 18123925−3620465 | +0.09 | −0.03 | +0.02 | −0.18 | 0.08 | 0.22 |
| 18110629−3632146 | +0.10 | −0.02 | +0.01 | −0.17 | 0.04 | 0.20 |
| 18133687−3639590 | +0.09 | −0.01 | −0.01 | −0.17 | 0.07 | 0.21 |
| 18111505−3620576 | +0.09 | −0.02 | +0.00 | −0.18 | 0.03 | 0.20 |
| 18120832−3628243 | +0.10 | −0.03 | +0.02 | −0.18 | 0.01 | 0.21 |
| 18130815−3631460 | +0.08 | −0.02 | +0.04 | −0.19 | 0.03 | 0.21 |
| 18120407−3636481 | +0.09 | −0.02 | +0.03 | −0.19 | 0.04 | 0.22 |
| 18135786−3640300 | +0.10 | −0.01 | +0.02 | −0.20 | 0.01 | 0.22 |
| 18131228−3619138 | +0.10 | −0.02 | +0.01 | −0.18 | 0.07 | 0.22 |
| 18113372−3650200 | +0.10 | −0.01 | +0.03 | −0.18 | 0.03 | 0.21 |
| 18115904−3650428 | +0.08 | −0.02 | +0.04 | −0.19 | 0.01 | 0.21 |
| 18115448−3641161 | +0.09 | −0.01 | +0.01 | −0.17 | 0.05 | 0.20 |
| 18123678−3649019 | +0.10 | −0.02 | +0.02 | −0.18 | 0.03 | 0.21 |
| 18113965−3645408 | +0.10 | −0.02 | +0.03 | −0.18 | 0.06 | 0.22 |
| 18135362−3636538 | +0.10 | −0.02 | +0.02 | −0.18 | 0.02 | 0.21 |
| 18123168−3631555 | +0.09 | −0.01 | +0.00 | −0.17 | 0.02 | 0.19 |
| 18115398−3623290 | +0.07 | −0.02 | +0.06 | −0.19 | 0.03 | 0.21 |
| 18123393−3615508 | +0.09 | −0.01 | +0.00 | −0.17 | 0.02 | 0.19 |
| 18120689−3643231 | +0.09 | +0.00 | +0.00 | −0.17 | 0.07 | 0.20 |
| 18130482−3649019 | ... | ... | ... | ... | ... | |
| 18110352−3646275 | +0.07 | −0.01 | +0.04 | −0.20 | 0.08 | 0.23 |
| 18105013−3629557 | +0.09 | −0.03 | +0.04 | −0.19 | 0.01 | 0.22 |
| 18121897−3630243 | +0.09 | −0.02 | +0.01 | −0.19 | 0.05 | 0.22 |
| 18122029−3652333 | +0.09 | −0.01 | +0.02 | −0.19 | 0.04 | 0.22 |
| (l, b) = (+8.5, +9) | ||||||
| 17311256−1702018 | +0.12 | −0.01 | −0.02 | −0.11 | 0.03 | 0.17 |
| 17290874−1632431 | +0.12 | −0.01 | −0.02 | −0.11 | 0.01 | 0.16 |
| 17302885−1639588 | +0.12 | −0.02 | −0.02 | −0.12 | 0.02 | 0.17 |
| 17304789−1623192 | +0.12 | −0.02 | −0.02 | −0.13 | 0.05 | 0.19 |
| 17321080−1641479 | +0.13 | −0.01 | +0.00 | −0.14 | 0.02 | 0.19 |
| 17303589−1638299 | +0.12 | −0.02 | −0.01 | −0.15 | 0.05 | 0.20 |
| 17290513−1630383 | +0.13 | −0.01 | +0.00 | −0.14 | 0.10 | 0.22 |
| 17314699−1654460 | +0.12 | −0.01 | −0.01 | −0.14 | 0.00 | 0.18 |
| 17305076−1615216 | +0.12 | −0.02 | −0.02 | −0.15 | 0.06 | 0.20 |
| 17323324−1627474 | ... | ... | ... | ... | ... | ... |
| 17312795−1631423 | +0.12 | +0.00 | −0.02 | −0.13 | 0.02 | 0.18 |
| 17290285−1638344 | +0.12 | +0.00 | −0.02 | −0.13 | 0.04 | 0.18 |
| 17303378−1703086 | +0.11 | −0.01 | +0.01 | −0.18 | 0.04 | 0.22 |
| 17304223−1609274 | +0.11 | −0.01 | +0.01 | −0.16 | 0.01 | 0.19 |
| 17304908−1633101 | +0.11 | −0.01 | +0.01 | −0.15 | 0.07 | 0.20 |
| 17291459−1650085 | +0.11 | −0.01 | +0.02 | −0.15 | 0.03 | 0.19 |
| 17300674−1638541 | +0.10 | −0.02 | +0.03 | −0.18 | 0.05 | 0.21 |
| 17315010−1653413 | +0.12 | −0.02 | +0.01 | −0.16 | 0.08 | 0.22 |
| 17295493−1613273 | +0.10 | −0.02 | +0.03 | −0.18 | 0.07 | 0.22 |
| 17311523−1618542 | ... | ... | ... | ... | ... | ... |
| 17314811−1621558 | +0.10 | +0.00 | +0.02 | −0.15 | 0.01 | 0.18 |
| 17304861−1646459 | +0.10 | −0.02 | +0.04 | −0.18 | 0.10 | 0.23 |
| 17323959−1625298 | +0.11 | −0.01 | +0.02 | −0.17 | 0.02 | 0.20 |
| 17285711−1633566 | +0.10 | −0.01 | +0.03 | −0.17 | 0.02 | 0.20 |
| 17314673−1641228 | +0.10 | −0.02 | +0.04 | −0.18 | 0.05 | 0.22 |
| 17294476−1626118 | +0.10 | −0.01 | +0.04 | −0.17 | 0.05 | 0.21 |
| 17320650−1643389 | +0.10 | −0.01 | +0.03 | −0.19 | 0.06 | 0.23 |
| 17314427−1640265 | +0.11 | −0.02 | +0.01 | −0.16 | 0.04 | 0.20 |
| 17300064−1701075 | +0.09 | −0.02 | +0.03 | −0.19 | 0.03 | 0.22 |
| 17302935−1652277 | +0.10 | −0.01 | +0.00 | −0.15 | 0.00 | 0.18 |
| 17320652−1619563 | +0.09 | −0.03 | +0.03 | −0.19 | 0.05 | 0.22 |
| 17304464−1631471 | +0.09 | −0.01 | +0.02 | −0.17 | 0.00 | 0.19 |
| 17321715−1632467 | +0.09 | +0.00 | +0.01 | −0.17 | 0.01 | 0.19 |
| 17321969−1653156 | +0.09 | −0.01 | +0.03 | −0.19 | 0.02 | 0.21 |
| 17315690−1630315 | +0.08 | −0.01 | +0.03 | −0.19 | 0.03 | 0.21 |
| 17312870−1619572 | +0.09 | −0.01 | +0.04 | −0.19 | 0.03 | 0.22 |
| 17294541−1649018 | +0.09 | −0.01 | +0.03 | −0.19 | 0.04 | 0.22 |
| 17305067−1644006 | +0.09 | +0.00 | +0.03 | −0.18 | 0.11 | 0.23 |
| 17312457−1652524 | +0.09 | −0.02 | +0.02 | −0.18 | 0.06 | 0.21 |
| 17292760−1636235 | +0.09 | −0.01 | +0.04 | −0.18 | 0.05 | 0.21 |
| 17295978−1633590 | +0.08 | +0.00 | +0.03 | −0.19 | 0.06 | 0.22 |
| 17322323−1649335 | +0.09 | −0.01 | +0.02 | −0.17 | 0.01 | 0.19 |
| 17321117−1654590 | +0.09 | −0.02 | +0.03 | −0.18 | 0.02 | 0.21 |
| 17313606−1607539 | +0.10 | −0.01 | +0.01 | −0.17 | 0.04 | 0.20 |
| 17295331−1653069 | +0.09 | −0.02 | +0.03 | −0.19 | 0.02 | 0.21 |
| 17302818−1636032 | +0.08 | −0.02 | +0.03 | −0.19 | 0.05 | 0.22 |
| 17293118−1638081 | +0.09 | −0.02 | +0.02 | −0.17 | 0.04 | 0.20 |
| 17291994−1618302 | +0.08 | +0.02 | +0.04 | −0.17 | 0.09 | 0.21 |
| 17320457−1646391 | +0.08 | −0.01 | +0.04 | −0.19 | 0.07 | 0.22 |
| 17310747−1620049 | +0.09 | −0.02 | +0.04 | −0.19 | 0.02 | 0.22 |
| 17323392−1636330 | +0.08 | −0.01 | +0.06 | −0.19 | 0.07 | 0.23 |
| 17312572−1609092 | +0.10 | −0.02 | +0.03 | −0.19 | 0.03 | 0.22 |
| 17300015−1609464 | +0.09 | −0.02 | +0.04 | −0.19 | 0.05 | 0.22 |
| 17305894−1637056 | +0.07 | +0.00 | +0.06 | −0.20 | 0.05 | 0.23 |
| 17291621−1647189 | +0.07 | +0.01 | +0.06 | −0.20 | 0.05 | 0.23 |
| 17302194−1643531 | +0.07 | +0.00 | +0.06 | −0.20 | 0.07 | 0.23 |
| 17311959−1643577 | +0.07 | −0.01 | +0.05 | −0.19 | 0.09 | 0.23 |
| 17311229−1659047 | +0.07 | +0.00 | +0.05 | −0.20 | 0.08 | 0.23 |
| 17313313−1659216 | +0.08 | −0.02 | +0.04 | −0.19 | 0.01 | 0.21 |
| 17301749−1629529 | +0.06 | −0.02 | +0.04 | −0.20 | 0.07 | 0.22 |
| 17294261−1622440 | +0.06 | −0.01 | +0.04 | −0.20 | 0.05 | 0.22 |
| 17323625−1637551 | +0.08 | −0.02 | +0.04 | −0.20 | 0.07 | 0.23 |
| 17314292−1620036 | +0.06 | +0.00 | +0.06 | −0.20 | 0.02 | 0.22 |
| 17310955−1635152 | +0.06 | +0.00 | +0.06 | −0.21 | 0.08 | 0.24 |
| 17304312−1630318 | +0.08 | −0.02 | +0.06 | −0.20 | 0.02 | 0.23 |
| 17285469−1627232 | +0.09 | −0.02 | +0.05 | −0.19 | 0.05 | 0.22 |
| 17310360−1700146 | +0.06 | −0.02 | +0.07 | −0.19 | 0.00 | 0.21 |
| 17295898−1652101 | +0.07 | −0.02 | +0.06 | −0.20 | 0.05 | 0.23 |
The abundance sensitivities to each model atmosphere parameter were calculated by varying each parameter independently. The procedure involved first using the best-fit model atmosphere parameters and abundances given in Tables 2 and 3 to calculate theoretical EWs for each line. These theoretical EWs were held fixed and then a new model atmosphere was created with the Teff, log(g), [M/H], or vt value varied by the amount given in Tables 5–8. However, it should be noted that the sensitivity of each line to changes in model atmosphere parameters are not necessarily the same. Therefore, the values given in Tables 5–8 represent the average difference between the newly derived abundances from each line and the original abundance given in Table 2.
The uncertainty ranges of ΔTeff = +100 K, Δlog(g) = +0.30, Δ[M/H] = +0.30, and Δvt = +0.30 km s-1 are likely to be conservative upper limits for each parameter. The Teff variations, based on the uncertainty in E(B − V), are typically small (<50 K) for almost all stars in our sample. In particular, the average differences between the Teff derived assuming the recommended E(B − V) and the maximum/minimum E(B − V) values are: +38 K (σ = 27 K)/−24 K (σ = 15 K) for the (−5.5, −7) field, +14 K (σ = 7 K)/−10 K (σ = 6 K) for the (−4, −9) field, and +21 K (σ = 12 K)/−22 K (σ = 10 K) for the (+8.5, +9) field. These values are significantly smaller than the 125 K 1σ value of the Alonso et al. (1999) J − KS color–temperature calibration. When we compare the Teff values derived using the Alonso et al. (1999) calibration to those derived using the González Hernández & Bonifacio (2009) calibration, we find our adopted Alonso et al. (1999) temperatures to be cooler by 63 K (σ = 8 K) in the (−5.5, −7) field, 68 K (σ = 7 K) in the (−4, −9) field, and 46 K (σ = 13 K) in the (+8.5, +9) field. Therefore, we believe that an estimated uncertainty of 100 K is a reasonable assumption for our data.
Since we did not calculate log(g) directly from photometry or ionization equilibrium, it is difficult to assess the true log(g) uncertainty. However, examination of Figure 2 suggests that the difference between our derived log(g) values and those in the literature is typically within ±0.30. For comparison, the Bescancon model22 (Robin et al. 2003) predicts that most bulge stars along our observed lines-of-sight should vary in distance by approximately ±2 kpc, though the full range may extend several kpc on either side of the Galactic center. This would lead to a maximum photometric log(g) uncertainty of ∼0.20–0.25. Note that oxygen, especially when normalized to Fe I, is the element most affected by log(g) uncertainties. Similarly, since surface gravity is proportional to log(M/M☉) for stars with the same Teff but different mass, it is likely that our abundance ratios will not be significantly altered by the possible inclusion of lower mass AGB stars in our sample.
As stated previously, the average line-to-line dispersion for Fe i is 0.16 dex, with a small dispersion of 0.03 dex. Similarly, we found that the use of α-enhanced versus solar-scaled models affected abundance ratios at ≲0.1 dex level. Therefore, it seems likely that the use of a model atmosphere [M/H] uncertainty of 0.3 dex should represent a conservative upper limit on the effects continuous opacity and electron number density have on derived abundances. From Tables 5–8, we find that [M/H] uncertainties have the largest effect (∼0.1 dex in magnitude) on O and Fe while Si and Ca abundances are less sensitive. The magnitude of the [M/H] uncertainty effect also tends to increase with increasing metallicity.
Our adopted microturbulence uncertainty of 0.3 km s-1 may also be a conservative estimate. For an individual star, the typical vt uncertainty based on removing any trends in Fe i abundance versus line strength is ∼0.1–0.15 km s-1. When comparing stars of similar metallicity (in 0.5 dex bins), the 1σ variation in derived vt values for stars of comparable temperature ranges from 0.17 km s-1 in the most metal-poor stars to 0.22 km s-1 in the most metal-rich stars. The effect of vt uncertainty on abundance is clear in Tables 5–8, which are sorted by metallicity in each field. Microturbulence becomes an increasingly important factor with increasing metallicity and thus line strength. Similarly, elements that were derived from stronger lines (e.g., Fe and Ca) are most sensitive to vt uncertainty.
3.5. Radial Velocity Determinations
Radial velocities for all stars were measured using the fxcor task in IRAF. For templates, we calculated synthetic spectra over the full wavelength range covered for each star. The synthetic spectra were produced using the model atmosphere parameters given in Table 2, and were smoothed and binned to match the dispersion of the object spectra. The average measurement error returned by fxcor was similar for all fields: 0.71 km s-1 (σ = 0.48 km s-1), 0.88 km s-1 (σ = 0.53 km s-1), and 0.62 km s-1 (σ = 0.38 km s-1) for the (−5.5, −7), (−4, −9), and (+8.5, +9) fields, respectively. The IRAF task rvcorrect was used the determine the heliocentric correction for all stars. The derived heliocentric radial velocities are provided in Table 2.
4. RESULTS AND DISCUSSION
4.1. Metallicity Distribution Functions
In Figure 7 we show the derived metallicity distribution functions for all three off-axis fields. These metallicity distributions are in reasonable agreement with those derived for similar outer bulge (∣b∣ >4°) minor-axis fields (Zoccali et al. 2008; Johnson et al. 2011; Ness et al. 2013; Uttenthaler et al. 2012). For the (−5.5, −7), (−4, −9), and (+8.5, +9) fields, we find a full range in [Fe/H] that spans −1.50 to +0.66 dex (σ = 0.47 dex), −1.40 to +0.26 dex (σ = 0.42 dex), and −1.26 to +0.59 dex (σ = 0.44 dex), respectively. As is the case with previous high resolution spectroscopic studies, we do not find any stars with [Fe/H] ≲ −1.5 that may be present in the bulge from the earliest epoch of star formation. This is in agreement with the ARGOS sample by Ness et al. (2013) that only found 0.71% (100/14147) of stars within 3.5 kpc of the Galactic center to have [Fe/H] <−1.5.
Figure 7. The top three panels show the metallicity distribution functions for all three bulge fields binned in 0.1 dex increments. The bottom panel compares the cumulative distribution functions for all three fields.
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Standard image High-resolution imageThe observed vertical metallicity gradient present along the bulge minor-axis, at least for ∣b∣ > 4° (Zoccali et al. 2008), appears to also be present in off-axis fields. This result is illustrated in Figure 8, where we show the metallicity distribution functions for four minor-axis and four off-axis fields at similar Galactic latitudes. In a similar fashion to the minor-axis trend, the median [Fe/H] ratios for the (+5, −3) field given in Gonzalez et al. (2011) and our (−5.5, −7) and (−4, −9) fields are [Fe/H] = −0.08, −0.29, and −0.44, respectively. The decline in the median [Fe/H] ratio with increasing Galactic latitude appears to be driven by the same phenomenon in both the minor-axis and off-axis fields. In particular, both sets of observations show a decrease in the relative fraction of metal-rich ([Fe/H] ≳ 0) stars, an increase in the relative fraction of the metal-poor ([Fe/H] ≲ −1) stars, and no significant change in the relative fraction of intermediate metallicity stars as a function of increasing Galactic latitude. This result is at least qualitatively in agreement with the scenario proposed by Babusiaux et al. (2010), in which the metallicity gradient is a reflection of the change in the bulge/bar population mixture at different Galactic latitudes (but see also Ness et al. 2013).
Figure 8. Metallicity distribution functions are shown for bulge RGB stars in four minor-axis (left panels) and four off-axis (right panels) fields. The dashed red line in each panel indicates the median [Fe/H] value. The (l, b) = (+1, −4), (0, −6), and (0, −12) fields are from Zoccali et al. (2008), the (0, −8) field is from Johnson et al. (2011), the (+5, −3) field is from Gonzalez et al. (2011), and the (−5.5, −7), (−4, −9), and (+8.5, +9) fields are from the present work. Note that the decreasing metallicity gradient with increasing Galactic latitude appears to be present along both the minor axis and off-axis.
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Standard image High-resolution imageThe data presented above indicate that the vertical metallicity gradient along l ∼ ±5° is approximately 0.4 dex kpc-1, which is similar to the minor-axis gradients found by Zoccali et al. (2008; 0.6 dex kpc-1) and Ness et al. (2013; 0.45 dex kpc-1).23 Given the uncertainty in bulge membership and possible biases of incomplete samples, it seems unlikely that the difference in magnitude (∼0.2 dex) between the derived metallicity gradients found here and in Zoccali et al. (2008) is significant. Additionally, there does not seem to be a strong radial [Fe/H] gradient in the bulge.
Interestingly, the northern bulge (+8.5, +9) field is slightly more metal-rich than the two southern fields, with a median [Fe/H] = −0.23. However, as can be seen in Figure 7, where we plot the cumulative [Fe/H] distribution functions for all fields, it is clear that the (+8.5, +9) and (−5.5, −7) fields share similar distributions. This is supported by the results of two-sided Kolmogorov–Smirnov (K-S) tests (Press et al. 1992), which indicate that there is insufficient evidence to reject the null hypothesis that the (+8.5, +9) and (−5.5, −7) are drawn from the same parent population (p-value = 0.881).24 On the other hand, the (−5.5, −7)/(−4, −9) and (−4, −9)/(+8.5, +9) field combinations are possibly drawn from different parent populations, with p-values of 0.031 and 0.045, respectively. It is not clear if this signifies an asymmetry in the bulge metallicity distribution between the northern and southern regions or is simply a result of the smaller sample size and slightly redder colors of the observed stars in the (+8.5, +9) field (see Figure 1). We also consider the possibility that the higher metallicity of the (+8.5, +9) field could be due to a predominance of the X-shaped bulge structure in that region. Ness et al. (2012) and Uttenthaler et al. (2012) suggest that the X-shaped bulge, traced by the double red clump, may be dominated by metal-rich ([Fe/H] >−0.5) stars. As can be seen in Saito et al. (2011; their Figure 3), one of the red clump components in the X-shaped structure appears prominently near our (+8.5, +9) sight line. A distant, lower density component is also noted near the (−5.5, −7) sight line, and the higher metallicity of both our (−5.5, −7) and (+8.5, +9) could partially reflect the predominance of the X-shaped structure in these fields.
4.1.1. Sample Selection Bias and Foreground Contamination
As mentioned in Section 2.1, the targets in all three bulge fields were selected from the blue side of the RGB to avoid cool stars with spectra that may be dominated by molecular bands (especially TiO). The naive interpretation is that this will produce a strong bias in our derived metallicity distribution functions and significantly undersample the most metal-rich stars. However, the bias may not be as strong as expected because several factors combine to disperse the observed J − KS–[Fe/H] relation including: differential reddening, a complicated spatial geometry with a distance spread that could range from ∼4.5–11.5 kpc in our fields,25 metallicity dependent [α/Fe] variations, a possible age range of ∼2–13 Gyr for stars with [Fe/H] ≳ −0.4 (e.g., see Figures 15 and 16 of Bensby et al. 2013; but see also Clarkson et al. 2008), and the mixing of RGB and AGB stars.
In general, it is not a trivial matter to estimate the observational bias of the color–metallicity relation in the bulge, especially in the J − KS and KS dimensions, because of large uncertainties in several of the factors listed above. This is evident both in the metallicity distribution functions produced here (Figure 7), which are not dominated by metal-poor stars as one might expect, and in the J − KS–[Fe/H] relations of previous studies that span a broader color range. In Figure 9 we show KS versus J − KS color–magnitude diagrams for the Zoccali et al. (2008) and Gonzalez et al. (2011) data sets and overplot the observed stars, with the most metal-poor ([Fe/H] <−0.7) and metal-rich ([Fe/H] >+0.2) subsets identified. While the differential reddening and distance distributions vary from field-to-field, a common feature among all fields is the significant mixing of metal-poor and metal-rich stars on the giant branch. The metal-rich population in particular appears to span the entire color range, although an unknown fraction of these stars may be disk and/or halo contaminators (see below).
Figure 9. Color–magnitude diagrams using 2MASS data (small black points) are shown for the bulge fields presented in Zoccali et al. (2008) and Gonzalez et al. (2011). The filled red circles are the observed stars in each field, those with magenta crosses are the most metal-poor stars ([Fe/H] <−0.7), and those with cyan crosses are the most metal-rich stars ([Fe/H] >+0.2). Note that both metal-poor and metal-rich stars are found over a broad range in J − KS color.
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Standard image High-resolution imageWhat is the effect on the derived metallicity distribution functions by preferentially sampling the blue side of the bulge giant branch? We can derive some estimate with the Zoccali et al. (2008) and Gonzalez et al. (2011) fields by comparing the metallicity distribution functions of the bluest third, which roughly matches our sample selection, to the full samples. The results are shown in Figure 10 where we plot histograms, cumulative distribution functions, provide results for two-sided K-S tests, compare the median [Fe/H] values, and compare the inter-quartile range (IQR) for each population. While it is clear from the cumulative distribution functions that (in most cases) the blue samples are moderately more metal-poor than the full samples, the effect is significantly smaller than anticipated. In fact, the two-sided K-S tests for all fields indicate that we cannot strongly reject the null hypothesis that the blue and full samples were drawn from the same parent population. Furthermore, the general shapes of the full metallicity distribution functions are preserved in the blue samples, and the median [Fe/H] and IQR values do not vary significantly between the two subsets, especially in the b > −4° fields that are most similar to our fields. In other words, the qualitative and quantitative results found especially by Zoccali et al. (2008), and particularly with regard to the [Fe/H] gradient, would not have been significantly altered by the selection of stars on the blue side of the giant branch.26
Figure 10. Metallicity distribution histograms and cumulative distribution functions are shown for the full samples (solid black lines) presented in Zoccali et al. (2008) and Gonzalez et al. (2011). Similar data are plotted using just the bluest third of each sample (solid blue lines), which roughly matches our sample selection. In the right panels we include the results of two-sided K-S tests (comparing the blue and total samples), median [Fe/H] values, and interquartile ranges (IQR) for each population.
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Standard image High-resolution imageFinally, we can compare our (−5.5, −7) and (−4, −9) fields with the data presented in Ness et al. (2013; their Figure 8). For the similar latitude minor-axis fields of (0, −7.5; 690 stars) and (0, −10; 650 stars) in Ness et al. (2013), they find median [Fe/H] values of −0.34 and −0.46, respectively. This is in good agreement with the median [Fe/H] values of our (−5.5, −7) and (−4, −9) fields, which have [Fe/H] = −0.29 and −0.44, respectively. The <0.05 dex difference between our derived median [Fe/H] values and Ness et al. (2013) is in agreement with the estimated bias introduced by the selection of stars on the blue side of the giant branch (see the middle panels of Figure 10). We conclude that our selection of bluer stars likely does not introduce a strong metallicity bias, and that the derived metallicity distribution functions are representative of the underlying population in each field. However, the metal-rich stars in our sample will be more concentrated on the near side of the bulge/bar system than a selection of stars with a broader color distribution.
In addition to the properties mentioned above that can blur the color–metallicity relation, contamination by disk and halo stars along the line-of-sight can also affect the derived metallicity distribution functions. While most studies agree that the halo contamination is small (≲2%; e.g., Zoccali et al. 2008; Hill et al. 2011; Uttenthaler et al. 2012), a true estimate of the (primarily) foreground thin and thick disk contamination is difficult to ascertain. In an attempt to gauge the impact of foreground contamination, the coordinates of stars in our two southern bulge fields were cross-referenced with the Southern Proper Motion IV catalog (SPM4; Girard et al. 2011).27 We were able to match 77/91 stars in the (−5.5, −7) field and 98/105 stars in the (−4, −9) field. Histograms of the proper motion results are shown in the top two panels of Figure 11. As can be seen in Figure 11, both fields contain a dominant population with a total proper motion ≲20 mas yr-1 and a tail that extends out to ∼35 mas yr-1 for the (−5.5, −7) field and ∼60 mas yr-1 for the (−4, −9) field. This is in good agreement with that found by Uttenthaler et al. (2012; their Figure 3) at (0, −10).
Figure 11. The left panels show (top) a histogram of the total proper motion for stars in the (−5.5, −7) field, (middle) a plot of (J − K)o vs. total proper motion, and (bottom) a plot of [Fe/H] vs. total proper motion. The right panels include the same information for the (−4, −9) field. The proper motion data are from the SPM4 catalog.
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Standard image High-resolution imageAs a rough estimate of contamination, we can assign targets lying in the tails of the proper motion distributions as possible foreground stars. Using a discriminator of 22 mas yr-1 for the (−5.5, −7) field and 21 mas yr-1 for the (−4, −9) field suggests foreground contamination rates of 9% (7/77) and 11% (11/98), respectively. However, given that many of the "outliers" fall within a few mas yr-1 of our cut–off and the proper motion errors are generally ∼3–8 mas yr-1, it is possible that as many as 50% of the possible outliers are actually bulge members. Additionally, since Uttenthaler et al. (2012) find that the double red clump and dual peaked metallicity distribution function features are present in their sample of stars with proper motions >20 mas yr-1, we follow their assessment and have not excluded any stars in our sample. We do note however that the middle and bottom panels of Figure 11, which plot (J − K)o and [Fe/H] versus total proper motion, give some indications that the more extreme proper motion outliers may clump together at colors and metallicities consistent with the foreground thin disk and metal-poor thick disk (or metal-rich halo).
4.2. Radial Velocities
In Figure 12 we plot histograms of the heliocentric radial velocity distributions for all fields analyzed here. The mean, median, and standard deviations are −26.6, −29.9, and 73.7 km s-1 for the (−5.5, −7) field, −40.7, −49.3, and 85.1 km s-1 for the (−4, −9) field, and −3.8, +15.2, and 81.6 km s-1 for the (+8.5, +9) field. Similarly, the mean/median galactocentric velocities (VGC) for these fields are: −40.8/−44.8 km s-1, −48.0/−57.8 km s-1, and +40.5/+60.2 km s-1. For the two southern bulge fields, the velocity distributions and dispersions are in good agreement with the BRAVA results (e.g., see Kunder et al. 2012; their Figure 11). This is confirmed in Figure 13 where we plot the velocity distributions from this work and overlapping or nearby BRAVA fields. A two-sided K-S test finds that the data are insufficient to strongly reject the null hypothesis that the (−5.5, −7)/(−6, −7) fields (p-value = 0.063) and (−4, −9)/(−4, −8) fields (p-value = 0.094) are drawn from the same parent populations. Additionally, the median galactocentric radial velocity and dispersion for our two southern bulge fields are in reasonable agreement with the Shen et al. (2010) bulge model, which find VGC = −52.2 (σ = 78.9) km s-1 and VGC = −54.1 (σ = 78.2) km s-1 at (l, b) = (−5.5, −7) and (−4, −9), respectively (Z. Li & J. Shen 2012, private communication).
Figure 12. The three panels show the heliocentric radial velocity distributions for each field in 10 km s-1 bins.
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Figure 13. The top left and bottom left panels compare the (−5.5, −7; red lines and symbols) and (−4, −9; blue lines and symbols) to nearby and/or overlapping fields observed for the BRAVA project (Howard et al. 2008; Kunder et al. 2012). The data are binned in 25 km s-1 increments. The right panel shows the Galactic longitude and latitude for individual stars in the new fields observed here, the comparison BRAVA fields used in the histograms (black crosses), and other nearby BRAVA fields (gray filled circles).
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Standard image High-resolution imageWhile the BRAVA sample did not extend to our single northern bulge field, the mean galactocentric velocity and dispersion we derived for the (+8.5, +9) field (VGC = +40.5 km s-1, σ = 81.6 km s-1) is in moderately good agreement with that found by Minniti (1996) for the nearby (+8, +7) field (VGC = +54.4 km s-1, σ = 84.4 km s-1). Similarly, our derived median galactocentric velocity for this field (VGC = +60.2 km s-1) is in reasonably good agreement with the Shen et al. (2010) median galactocentric velocity model value of VGC = +71.6 km s-1 (σ = 65.7 km s-1; Z. Li & J. Shen 2012, private communication). As was mentioned in Section 4.1, it is possible that the (+8.5, +9) sight line may be partially contaminated by one of the structures associated with the X-shaped bulge (e.g., see Saito et al. 2011; their Figure 3). This could result in additional substructure being present in our empirical velocity distribution function. However, visual inspection of Figure 12 does not indicate strong evidence of any additional features. This is supported by the results of Shapiro–Wilk and Anderson–Darling normality tests, which return p-values of 0.288 and 0.114 and indicate insufficient evidence to reject the null hypothesis that the (+8.5, +9) velocity distribution is normal.
In Figure 14 we show the heliocentric radial velocity and dispersion distributions as a function of [Fe/H] for all fields. As can be clearly seen in Figure 14, all three fields exhibit nearly identical trends of a decreasing velocity dispersion with increasing [Fe/H]. This observed trend is consistent with both the red clump and giant data analyzed in other outer bulge (∣b∣ ≳ 6°) fields (e.g., Minniti 1996; Babusiaux et al. 2010; de Propris et al. 2011; Johnson et al. 2011; Uttenthaler et al. 2012), and contrasts with the minor-axis results found by Babusiaux et al. (2010; their Figure 6) at b = −4° (opposite trend) and b = −6° (no trend). While de Propris et al. (2011) also find a correlation between the mean radial velocity and [Fe/H] for red clump stars, Babusiaux et al. (2010) and Uttenthaler et al. (2012) do not find significant evidence of mean velocity variations as a function of metallicity. Visual inspection of Figure 14 indicates that we also do not find significant variations in mean/median velocity as a function of [Fe/H] with two exceptions: (1) the metal-poor ([Fe/H] <−1) stars in all fields and (2) the intermediate metallicity (−0.5 ≲ [Fe/H] ≲ 0) stars in the (+8.5, +9) field.
Figure 14. The left panels show the heliocentric radial velocity distribution as a function of [Fe/H] for the (−5.5, −7) (filled red circles), (−4, −9) (filled blue circles), and (+8.5, +9) (filled green circles) fields. In the right panel, the velocity dispersion is shown for all three fields with the data merged into 0.5 dex [Fe/H] bins. The larger error bars on the most metal-poor bin are due to the relatively small sample size.
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Standard image High-resolution imageWhen the data are partitioned into 0.5 dex [Fe/H] bins, the median radial velocities within each bin of the (−5.5, −7) and (−4, −9) fields vary by <20 km s-1 (ignoring the [Fe/H] <−1 stars). The same is also true in the (+8.5, +9) field where the stars with −1 < [Fe/H] <−0.5 and [Fe/H] > 0 have median radial velocities of −24.6 and −28.4 km s-1, respectively. However, the stars in this field with −0.5 < [Fe/H] < 0 exhibit a noticeable velocity increase to +28.8 km s-1. Although there is evidence that the X-shaped bulge structure traced by the double red clump may preferentially contain stars with [Fe/H] >−0.5 (Ness et al. 2012; Uttenthaler et al. 2012), it is not clear if the increase in median velocity near [Fe/H] ∼−0.5 for our RGB sample is due to contamination from the nearby X-shape structure or is simply a statistical fluctuation.
For the metal-poor ([Fe/H] <−1) stars in the (−5.5, −7), (−4, −9), and (+8.5, +9) fields the median heliocentric velocities are: +49.6 (σ = 119.2) km s-1, −70.8 (σ = 117.4) km s-1, and −114 (σ = 109.3) km s-1, respectively. This contrasts with the more homogeneous set of stars with [Fe/H] >−1, which have median velocities and dispersions of −32.5 (σ = 66.1) km s-1, −42.1 (σ = 79.4) km s-1, and +17.4 (σ = 76.1) km s-1. However, the relatively small number of stars in the most metal-poor bin of each field makes it difficult to assess the significance of the larger median velocities and dispersion of these stars. Therefore, we instead attempt to determine how many of the stars with [Fe/H] <−1 might be outliers by using the interquartile range (IQR) of the more metal-rich ([Fe/H] >−1) stars in each field. We define moderate outliers as stars with velocities of 1.5–3.0×IQR above/below the median and extreme outliers as stars having velocities >3.0×IQR above/below the median. While we did not find extreme outliers in any of the fields, ∼20%–40% of the metal-poor stars are moderate outliers and may belong to the halo. The small percentage of stars with both low [Fe/H] and high velocities is consistent with the halo contamination estimate given in Section 4.1.1.
4.3. α-Element Abundances
While iron may be produced by both short lived Type II supernovae (SNe) and longer lived Type Ia SNe, the α elements are primarily produced only by massive stars. As a consequence, the [α/Fe] ratio can be a useful diagnostic for determining the chemical enrichment history of a stellar population (e.g., Tinsley 1979; Matteucci & Brocato 1990). In particular, the magnitude of the [α/Fe] ratios and the metallicity at which the [α/Fe] ratio begins to decline (presumably due to the onset of Type Ia contributions) yield information about important quantities such as a population's initial mass function (IMF) and star formation rate (e.g., see review by McWilliam 1997 and references therein). Additionally, the star-to-star dispersion of the measured [α/Fe] ratios in a given metallicity range can provide insight regarding the homogeneity of the gas from which the observed stars formed. In order to help address these issues in the bulge, we have measured the [O/Fe], [Si/Fe], and [Ca/Fe] ratios for stars in all three of our bulge fields.
In Figures 15–17 we plot [O/Fe], [Si/Fe], and [Ca/Fe] as a function of [Fe/H], respectively. To first order, all of the [X/Fe] ratios follow the same general trend of being enhanced by ≳ +0.3 dex at [Fe/H] ≲ −0.5 and then declining monotonically with increasing [Fe/H]. However, despite all of the α-elements sharing the same [Fe/H] value at which a steeper decline in their [X/Fe] ratios occurs, it is clear from Figures 15–17 that each element exhibits a slightly different trend. In particular, we note: (1) the [O/Fe] ratios are ∼0.1–0.3 dex larger than either [Si/Fe] or [Ca/Fe] for a given [Fe/H], (2) the decline in [Ca/Fe] with increasing [Fe/H] is more shallow than for [O/Fe] and [Si/Fe], (3) the [Si/Fe] data appear to continuously decline at [Fe/H] > 0 while the [O/Fe] and [Ca/Fe] distributions appear to flatten out, and (4) the difference between the median [X/Fe] ratios for stars with [Fe/H] <−0.5 and [Fe/H] >−0.5 is marginally larger for [O/Fe] than either [Si/Fe] or [Ca/Fe] (see also Table 9). This last point has been noted previously (e.g., McWilliam & Rich 2004; Zoccali et al. 2006; Fulbright et al. 2007; Alves-Brito et al. 2010; Ryde et al. 2010), and may be related to mass loss in Wolf–Rayet stars, rapidly rotating massive metal-poor stars, or metal-poor binary systems (e.g., McWilliam et al. 2008; Cescutti et al. 2009; but see also Ryde et al. 2010 and Alves-Brito et al. 2010). Unfortunately, we did not measure C, N, or Mg in our spectra and cannot comment further on the likelihood of our measured [O/Fe] abundances being affected by mass and/or metallicity-dependent reductions in the oxygen yield from massive stars.
Figure 15. [O/Fe] is plotted as a function of [Fe/H] for all three fields. For display purposes, the individual error bars are suppressed in the bottom panel and a typical error bar is shown in the top right corner.
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Figure 16. Similar to Figure 15 with [Si/Fe] plotted as a function of [Fe/H].
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Figure 17. Similar to Figure 15 with [Ca/Fe] plotted as a function of [Fe/H].
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Standard image High-resolution imageInterestingly, the individual abundance trends are nearly identical in all three of our fields, an observation that is highlighted in the bottom panels of Figures 15–17. The similarities between the different fields is also evident by examining Table 9, which summarizes the median [X/Fe] ratios and star-to-star dispersions for the metal-poor ([Fe/H] <−0.5) and metal-rich ([Fe/H] >−0.5) groups in each field. The dispersion value, listed as σ in Table 9, represents the scatter around a best-fit line through each subpopulation, and is likely a fair representation of the measurement error. On average, the scatter for [O/Fe], [Si/Fe], and [Ca/Fe] only increases by +0.06, +0.02, and +0.02 dex between the metal-poor and metal-rich populations. These data support previous observations (e.g., Gonzalez et al. 2011; Johnson et al. 2011; Rich et al. 2012; Uttenthaler et al. 2012) that the bulge was well-mixed across a large volume and that large-scale IMF and star formation history differences were either not present or were diluted by mixing.
Table 9. α-element Abundance Summary
| Field | [O/Fe] | σ | [Si/Fe] | σ | [Ca/Fe] | σ |
|---|---|---|---|---|---|---|
| Median | Median | Median | ||||
| [Fe/H] <−0.5 | ||||||
| (−5.5, −7) | +0.61 | 0.14 | +0.31 | 0.07 | +0.30 | 0.11 |
| (−4, −9) | +0.57 | 0.14 | +0.38 | 0.16 | +0.33 | 0.11 |
| (+8.5, +9) | +0.59 | 0.11 | +0.38 | 0.09 | +0.27 | 0.10 |
| [Fe/H] >−0.5 | ||||||
| (−5.5, −7) | +0.14 | 0.18 | −0.03 | 0.13 | +0.09 | 0.12 |
| (−4, −9) | +0.22 | 0.19 | +0.13 | 0.12 | +0.21 | 0.13 |
| (+8.5, +9) | +0.27 | 0.22 | +0.02 | 0.11 | +0.05 | 0.14 |
Notes. The σ values listed in the table represent the scatter around a best fit line to either the [Fe/H] <−0.5 or [Fe/H] >−0.5 stars in each field.
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In order to examine further the small differences between the various α-element trends, we compare our abundances with three bulge chemical enrichment models in Figure 18. The models in Figure 18 include the primary bulge model from Kobayashi et al. (2011; solid red line), a model assuming a flat IMF (x = 0.3; dashed green line), and a model assuming a flat IMF with both outflow (to reduce the Fe production) and a larger binary fraction than the solar neighborhood (dotted blue line). We find that the individual α-element abundance trends are fit reasonably well by the nominal Kobayashi et al. (2011) model that assumes a Kroupa (2008) IMF (x = 1.3) for massive stars, rapid star formation (shorter than the solar neighborhood), and a short star formation duration (∼3 Gyr). On the other hand, the one-zone flat IMF model clearly fails to reproduce the observed decrease in the [X/Fe] ratios with increasing [Fe/H], unless gas outflow is included to decrease the Fe yield. From these data we can conclude that: (1) a flat IMF model that does not include outflow (or some other way to decrease Fe production) fails to match the universal decline in [α/Fe] at [Fe/H] ≳ − 0.5 observed in our bulge fields, (2) the data are consistent with a model in which a significant portion of the bulge formed rapidly (<3 Gyr) and with a majority of its chemical enrichment driven by massive stars, and (3) the variations in the [X/Fe] versus [Fe/H] trends between the individual α-elements are consistent with our current understanding of massive star nucleosynthesis. Although the Kobayashi et al. (2011) model is able to provide a reasonable fit to our [O/Fe] and [Ca/Fe] data, we note that the model values for [Si/Fe] have been artificially reduced by −0.2 dex to provide a consistent fit. It is not clear if the Si offset is due to problems related to the nucleosynthesis codes (e.g., reaction rates; treatments of convection), the abundance codes (e.g., NLTE/3D effects; model atmosphere deficiencies), or both.
Figure 18. The [O/Fe], [Si/Fe], and [Ca/Fe] abundances for all three fields (combined) are plotted as a function of [Fe/H]. The solid red line shows the predicted change in each α element as a function of [Fe/H], based on the bulge model of Kobayashi et al. (2011). The dashed green line is the model prediction assuming a flatter IMF (x = 0.3) and the dotted blue line is the model prediction assuming x = 0.3 with outflow. Note that the [Si/Fe] model values have been systematically decreased by 0.2 dex (see text for details).
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Standard image High-resolution image4.3.1. Comparison with Other Bulge Fields
Several past studies have examined the behavior of various α-elements in fields along both the minor and major axis of the bulge (McWilliam & Rich 1994; Rich & Origlia 2005; Cunha & Smith 2006; Zoccali et al. 2006; Fulbright et al. 2007; Lecureur et al. 2007; Rich et al. 2007a; Meléndez et al. 2008; Alves-Brito et al. 2010; Bensby et al. 2010b, 2011, 2013; Ryde et al. 2010; Gonzalez et al. 2011; Hill et al. 2011; Johnson et al. 2011; Ness et al. 2013; Rich et al. 2012; Uttenthaler et al. 2012). All of these studies tend to find that metal-poor ([Fe/H] ≲ −0.5) stars universally show enhancements of at least +0.3 dex in their [α/Fe] ratios, with the more metal-rich stars exhibiting lower [α/Fe] ratios. Additionally, despite differing data quality, instruments, and measurement techniques, a general consensus has emerged indicating that the [α/Fe] versus [Fe/H] trends are essentially identical among all bulge fields and that this may be especially true among bulge stars with [Fe/H] ≲ −0.5.
In Figure 19 we overplot our derived [O/Fe], [Si/Fe], and [Ca/Fe] abundances as a function of [Fe/H] with those available in the literature. Except for small offsets (≲0.1 dex) due to systematic differences in abundance scales, our data are generally in good agreement with those available in other bulge fields. The lone exception appears to be the [Si/Fe] abundances at [Fe/H] ≳ 0. In particular, our [Si/Fe] ratios appear to decline more rapidly with increasing [Fe/H] than those found in other fields. Unfortunately, the reason for this discrepancy is not immediately clear, but it could result from effects such as the high excitation potential of the Si i lines used here or the sensitivity of especially the 6155 Å Si i line to CN contamination in cool, metal-rich giants (see Figure 6). We note that there do not appear to be any strong trends between [Si/Fe] and Teff or between abundances derived from the 6145 and 6155 Å Si i lines. Alternatively, the data may reflect a true [Si/Fe] abundance difference between metal-rich stars on the minor/major bulge axes and in off-axis fields. However, this seems less likely given the agreement between our data and the literature for [O/Fe] and [Ca/Fe] at [Fe/H] > 0. In any case, the majority of our data, including the [Si/Fe] ratios at [Fe/H] < 0, extend the findings of previous work (e.g., Gonzalez et al. 2011), indicating that there is no significant α-element gradient present in the bulge.
Figure 19. [O/Fe], [Si/Fe], and [Ca/Fe] ratios are plotted as a function of [Fe/H] for all bulge stars measured here (filled gray circles) and compared with previous bulge measurements (filled blue circles). The individual error bars have been suppressed for display purposes and a typical error bar is shown in the top right corner of each panel. The literature data are from: McWilliam & Rich (1994), Rich & Origlia (2005), Fulbright et al. (2007), Lecureur et al. (2007), Rich et al. (2007a), Meléndez et al. (2008), Alves-Brito et al. (2010), Bensby et al. (2010b), Ryde et al. (2010), Bensby et al. (2011), Gonzalez et al. (2011), Johnson et al. (2011), and Rich et al. (2012).
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Standard image High-resolution image4.3.2. Comparison with the Galactic Halo and Disk
As mentioned in Section 1, early comparisons of the bulge's chemical composition to the other major Galactic stellar populations (i.e., disk and halo) seemed to indicate that bulge stars may be uniquely enhanced in their [α/Fe] ratios (Zoccali et al. 2006; Fulbright et al. 2007; Lecureur et al. 2007), but recent studies have instead found that the bulge may be chemically similar to the thick disk and possibly metal-rich tail of the halo (Prochaska et al. 2000; Meléndez et al. 2008; Bensby et al. 2010a, 2010b, 2011; Ryde et al. 2010; Alves-Brito et al. 2010; Gonzalez et al. 2011; Hill et al. 2011; Johnson et al. 2011). However, it is not yet clear if the chemical similarity, particularly between the bulge and thick disk, extends to other light and heavy elements as well (e.g., Fulbright et al. 2007; Lecureur et al. 2007; Alves-Brito et al. 2010; Johnson et al. 2012).
In Figures 20–22 we compare our derived [O/Fe], [Si/Fe], and [Ca/Fe] abundances to those available in the literature for both giants and dwarfs in the halo, thick disk, and thin disk.28 First examining [O/Fe] for stars with [Fe/H] < 0, Figure 20 shows that the thick disk and halo exhibit nearly identical abundance patterns with respect to the bulge, albeit with a smaller star-to-star scatter. Further inspection of Figure 20 also reveals that our most metal-poor bulge stars may have slightly enhanced (∼0.1–0.2 dex) [O/Fe] ratios relative to similar metallicity halo and thick disk giants. However, we do not believe this offset is significant because: (1) previous differential analyses have found good agreement for [O/Fe] between these populations (e.g., Meléndez et al. 2008; Alves-Brito et al. 2010), (2) ∼0.1 dex of the offset is due to a zero point difference between this work and Alves-Brito et al. (2010; the green crosses in Figure 20), and (3) the observed difference is within the error bars of our [O/Fe] measurements. While the thin disk stars with [Fe/H] ≲ 0 exhibit lower [O/Fe] ratios than the bulge, the situation becomes less clear at higher [Fe/H]. For super-solar metallicities the [O/Fe] abundance trends of the thin disk, thick disk, and bulge appear to merge and may become indistinguishable.
Figure 20. [O/Fe] ratios are plotted as a function of [Fe/H] for bulge stars in all three fields (filled gray circles), the Galactic halo (top panels), thick disk (middle panels), and thin disk (bottom panels). For the halo and disk populations, abundances derived from dwarfs and/or subgiants are designated by magenta open boxes and abundances derived from giants are designated by green crosses. The individual error bars for our bulge stars have been suppressed for display purposes and a typical error bar is shown in the top right corner of each panel. The halo and disk data are from: Tomkin et al. (1992), Edvardsson et al. (1993), Prochaska et al. (2000), Reddy et al. (2003), Bensby et al. (2005), Brewer & Carney (2006), Reddy et al. (2006), and Alves-Brito et al. (2010). For the Alves-Brito et al. (2010) giant data we show only the abundances derived using Kurucz atmospheres.
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Standard image High-resolution imageFor the [Si/Fe] versus [Fe/H] distributions shown in Figure 21, we again find that the halo and thick disk, especially at [Fe/H] < 0, are nearly identical to that of the bulge. However, much like the [O/Fe] distributions, any similarities between the bulge and thick disk become difficult to assess at [Fe/H] > 0. The number of thick disk giants in this metallicity regime for which [Si/Fe] has been measured is too small to draw any firm conclusions. In contrast, the [Si/Fe] ratios of the thin disk stars with [Fe/H] ≲ 0 are underabundant relative to the bulge, and neither the dwarf nor giant trends exhibit the continued decline in [Si/Fe] at [Fe/H] > 0 seen in both our data and possibly those of other bulge studies (see Figure 19).
While the halo [Ca/Fe] abundances derived from both dwarfs and giants are in excellent agreement with our bulge values, the thick disk [Ca/Fe] ratios for stars with [Fe/H] ≲ −0.3 are ∼0.1 dex lower. Similarly, the thin disk [Ca/Fe] abundances for stars with [Fe/H] < 0 are considerably lower than those found in the bulge. However, the [Ca/Fe] abundance differences between the thin disk, thick disk, and bulge again become difficult to untangle at [Fe/H] > 0 (see Figure 22). For the more metal-poor thick disk giant sample, we can partially reconcile the [Ca/Fe] abundance difference by applying the ∼0.05 dex zero point offset between our abundance scale and that used by Alves-Brito et al. (2010). The zero point correction also affects the thin disk and halo giant samples, but does not alter our conclusions regarding the chemical similarities between these populations.
Figure 21. Similar to Figure 20 with [Si/Fe] plotted as a function of [Fe/H]. The halo and disk data are from: Edvardsson et al. (1993), Nissen & Schuster (1997), Fulbright (2000), Prochaska et al. (2000), Stephens & Boesgaard (2002), Johnson (2002), Bensby et al. (2003), Reddy et al. (2003), Bensby et al. (2005), Brewer & Carney (2006), Reddy et al. (2006), and Alves-Brito et al. (2010).
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Standard image High-resolution imageIn summary, we find in agreement with recent studies that the metal-poor component of the bulge ([Fe/H] ≲ 0) and thick disk share indistinguishable [α/Fe] abundance distributions, and that these similarities are independent of the α-element analyzed. Additionally, we find that the most metal-poor ([Fe/H] <−1) stars in the bulge also exhibit very similar [α/Fe] distributions to the more metal-rich stars in the halo. However, we note that this may not be surprising given that some of our metal-poor bulge stars could be halo interlopers (see Section 4.1.1). In contrast, the thin disk stars are generally underabundant in their [α/Fe] ratios compared to bulge stars, at least for [Fe/H] < 0. For the most metal-rich stars in the bulge, the [O/Fe] and [Ca/Fe] data suggest that there may be significant chemical overlap with the thin disk and/or metal-rich tail of the thick disk. While our data and those from past studies indicate that the bulge and especially thick disk may have shared similar chemical enrichment histories, more work is needed to determine how these two populations are linked.
5. SUMMARY
We have determined [Fe/H], [O/Fe], [Si/Fe], and [Ca/Fe] abundance ratios, as well as radial velocities, for 264 RGB stars in three off-axis bulge fields centered near (l, b) = (−5.5, −7), (−4, −9), and (+8.5, +9). The abundances were derived from moderate resolution (R ≈ 18,000), high S/N (∼75–300 pixel-1) spectra obtained with the Hydra multiobject spectrographs on the Blanco 4m and WIYN 3.5 m telescopes. While the [Fe/H] abundances were measured using equivalent width analyses, the [O/Fe], [Si/Fe], and [Ca/Fe] abundances were measured using spectrum synthesis techniques. The stars were selected from the blue side of the giant branch, but an analysis of the color–metallicity relation in other bulge samples that span a broader color range suggests this may not introduce a strong metallicity bias.
The metallicity distribution functions for all three fields are in general agreement with those found in minor-axis, outer bulge fields. In particular, the full range in [Fe/H] found in each field spans from roughly [Fe/H] = −1.5 to +0.5 dex, and the median metallicity for the two southern bulge fields decreases with increasing Galactic latitude. Combining our (−5.5, −7) and (−4, −9) metallicity distributions with the Gonzalez et al. (2011) data at (+5.25, −3) indicates that the vertical metallicity gradient observed by Zoccali et al. (2008) along the minor-axis is also present in off-axis fields. We find a similar [Fe/H] gradient of ∼0.4 dex kpc-1. However, there does not seem to be a similarly strong radial [Fe/H] gradient. Interestingly, the northern bulge field at (+8.5, +9) was found to have the highest median metallicity ([Fe/H] = −0.23) sample. However, it is not clear if this is a selection effect resulting from redder stars being observed in this field, an indication of asymmetry in the metallicity distribution of the bulge, or possible contamination in the field by the X-shaped (and possibly metal-rich) bulge structure.
The radial velocities and dispersion derived here are in good agreement with the BRAVA survey, and by extension are in reasonable agreement with the Shen et al. (2010) model. All three of our fields are also found to exhibit nearly identical radial velocity dispersion versus [Fe/H] relations that show a strong decrease in dispersion with increasing metallicity. This trend matches previous observations of outer bulge fields, but contrasts with the dispersion–metallicity relation found at ∣b∣ <6°. In the two southern bulge fields, we do not find any significant variations with respect to the median velocity as a function of [Fe/H]. The same is also true for the more metal-poor and metal-rich stars in the northern field, but there is an unexpected increase in median velocity for stars with −0.5 < [Fe/H] < 0 in this field. It is possible that this effect could be tied to the X-shaped bulge structure that resides near the (+8.5, +9) sight line.
We find in agreement with past studies that the [α/Fe] ratios are enhanced in all bulge fields at [Fe/H] ≲ −0.5, but the α-element abundances monotonically decline at higher metallicities. Additionally, the [O/Fe], [Si/Fe], and [Ca/Fe] abundance trends exhibit remarkable homogeneity across all fields analyzed in this work and previous studies. A significant [α/Fe] abundance gradient does not appear to exist in the bulge. Small variations in the slope and magnitude of the individual α-element trends are consistent with our current understanding of massive star nucleosynthesis, and support the idea that the bulge was well-mixed and formed more rapidly than the local thin disk. However, we find in agreement with several recent studies that for [Fe/H] ≲ 0 the bulge [α/Fe] ratios are indistinguishable from the halo and thick disk. Unfortunately, it is not yet clear if the similar [α/Fe] trends between especially the bulge and thick disk extend to super-solar metallicities.
Figure 22. Similar to Figure 20 with [Ca/Fe] plotted as a function of [Fe/H]. The literature data are from the same sources as in Figure 21.
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This research has made use of NASA's Astrophysics Data System Bibliographic Services. This material is based upon work supported by the National Science Foundation under award No. AST–1003201 to C.I.J. C.A.P. gratefully acknowledges support from the Daniel Kirkwood Research Fund at Indiana University. R.M.R. acknowledges support from NSF grant AST–0709479 and AST–121120995. A.K. thanks the Deutsche Forschungsgemeinschaft for funding from Emmy-Noether grant Ko 4161/1.
Footnotes
- 9
Some results from the ARGOS study are presented in Ness et al. (2013), but the individual abundances are not yet publicly available.
- 10
We make use of the standard spectroscopic notation where [A/B]≡log(NA/NB)star–log(NA/NB)☉ and log
(A)≡log(NA/NH)+12.0 for elements A and B. - 11
IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation.
- 12
- 13
The 2MASS J and KS values were converted onto the TCS system, as required for using the Alonso et al. (1999) color–temperature relation.
- 14
The E(B − V) values can be accessed at: http://irsa.ipac.caltech.edu/applications/DUST/.
- 15
The isochrones can be accessed at: http://stellar.dartmouth.edu/models/grid.html.
- 16
The model atmosphere grid can be accessed at: http://wwwuser.oat.ts.astro.it/castelli/grids.html.
- 17
The Arcturus atlas can be accessed at: http://www.noao.edu/archives.html.
- 18
Based on spectral data retrieved from the ELODIE archive at Observatoire de Haute-Provence (OHP). The ELODIE archive can be accessed at: http://atlas.obs-hp.fr/elodie/.
- 19
The NIST database can be accessed at: http://www.nist.gov/pml/data/asd.cfm.
- 20
VALD can be accessed at: http://vald.astro.univie.ac.at/~vald/php/vald.php.
- 21
The Kurucz line list database can be accessed at: http://kurucz.harvard.edu/linelists.html.
- 22
The Bescancon model form can be accessed at: http://model.obs-besancon.fr/.
- 23
Note that Ness et al. (2013) also argue that the metallicity gradient of the individual bulge components they have identified may be significantly more shallow, on the order of 0.07 dex kpc-1, than the 0.4–0.6 dex kpc-1 found here and in previous studies. Unfortunately, our sample sizes are insufficient to attempt a similar multi-component deconvolution of the distribution functions shown in Figure 7.
- 24
We adopt the common interpretation that the null hypothesis can be rejected if p < 0.05.
- 25
This estimate is based on the Bescancon model.
- 26
We tested for the effects of differential reddening and photometric errors in the 2MASS J and KS data but did not find significant changes to the distribution functions or median [Fe/H] and IQR values.
- 27
The stars in our northern bulge field have a declination of ∼ −16°, which is outside the SPM4 range of −20° to −90°.
- 28
As has been noted in past work (e.g., Alves-Brito et al. 2010), a direct comparison between abundance trends derived from giant and dwarf spectra may be contaminated by zero-point offsets that can reach at least the 0.1–0.2 dex level. Therefore, in Figures 20–22 we include both giant and dwarf data for comparison, but caution that apparent systematic abundance differences ≲0.1 dex in the [α/Fe] ratios may not be significant.