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Erratum: "Chemical Abundances of New Member Stars in the Tucana II Dwarf Galaxy" (2018, ApJ, 857, 74)

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Published 2018 June 14 • © 2018. The American Astronomical Society. All rights reserved.
, , Citation Anirudh Chiti et al 2018 ApJ 860 86 DOI 10.3847/1538-4357/aac48f

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achiti@mit.edu

Author affiliations

1 Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA; achiti@mit.edu

2 Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA

3 Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia

4 Astronomy Department, University of California, Berkeley, CA, USA

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5 Hubble Fellow.

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Dates

  1. Received 2018 May 9
  2. Accepted 2018 May 11
  3. Published

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0004-637X/860/1/86

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The coordinates for TucII-078 in Table 1 and the location of TucII-078 in the right panel of Figure 2 were incorrect. The correct coordinates for TucII-078 are now listed in Table 1 and the correct location of the star is shown in the right panel of Figure 2. There were no other references to the coordinates of this star in the text.

Figure 2.

Figure 2. Left: color–magnitude diagram of Tuc II stars from this study. A Dartmouth isochrone (Dotter et al. 2008) with an age of 12.5 Gyr, distance modulus of 18.8, and a metallicity of [Fe/H] = −2.5 is overplotted in black along with offsets of (g−r) ± 0.1 in dashed lines to guide the eye. We denote with different colors the four members previously observed by Ji et al. (2016), one member selected from Walker et al. (2016), and two selected from our SkyMapper photometry. Open circles indicate confirmed members in Walker et al. (2016) with no high-resolution spectroscopic observations. Right: spatial distribution of Tuc II members centered on the coordinates of Tucana II. The elliptical half-light radius from Koposov et al. (2015) is overplotted. In both plots, each star is labeled by its identifier as found Table 1.

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Table 1.  Observations

Name R.A. (h:m:s) (J2000) Decl. (d:m:s) (J2000) Slit Size g (mag) ${t}_{\exp }$ (minutes) S/Na ${v}_{\mathrm{helio}}$ (km s−1)
TucII-006 22:51:43.06 −58:32:33.7 1farcs0 18.78 206b 15, 30 −126.1
TucII-011 22:51:50.28 −58:37:40.2 1farcs0 18.27 314b 15, 30 −124.6
TucII-033 22:51:08.32 −58:33:08.1 1farcs0 18.68 155b 17, 32 −126.9
TucII-052 22:50:51.63 −58:34:32.5 1farcs0 18.83 155b 17, 35 −119.9
TucII-078 22:50:41.07 −58:31:08.3 1farcs0 18.62 215 15, 30 −123.8
TucII-203 22:50:08.87 −58:29:59.1 1farcs0 18.81 275 16, 37 −126.1
TucII-206 22:54:36.67 −58:36:57.9 1farcs0 18.81 385 15, 37 −122.9

Notes.

aS/N per pixel is listed for 4500 and 6500 Å. bCombined exposure time from Ji et al. (2016) and this work.

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10.3847/1538-4357/aac48f