ERRATUM: “THE DISK POPULATION OF THE TAURUS STAR-FORMING REGION” (2010, ApJS, 186, 111)

K. L. Luhman; P. R. Allen; C. Espaillat; L. Hartmann; N. Calvet

doi:10.1088/0067-0049/189/2/353

The Astrophysical Journal Supplement Series

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ERRATUM: "THE DISK POPULATION OF THE TAURUS STAR-FORMING REGION" (2010, ApJS, 186, 111)

K. L. Luhman^1,2, P. R. Allen¹, C. Espaillat^4,3, L. Hartmann³, and N. Calvet³

Published 2010 August 3 • © 2010. The American Astronomical Society. All rights reserved.
The Astrophysical Journal Supplement Series, Volume 189, Number 2 Citation K. L. Luhman et al 2010 ApJS 189 353 DOI 10.1088/0067-0049/189/2/353

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This is a correction for 2010 ApJS 186 111

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kluhman@astro.psu.edu

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¹ Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA; kluhman@astro.psu.edu

² Center for Exoplanets and Habitable Worlds, The Pennsylvania State University, University Park, PA 16802, USA

³ Department of Astronomy, The University of Michigan, Ann Arbor, MI 48109, USA

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⁴ Current address: Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA.

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Published 2010 August 3

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In Table 7, we inadvertently omitted the spectral type bins in which class II sources were placed in Table 8 based on their bolometric luminosities (this applies only to stars that lack spectroscopic classifications). The bins were K6–M3.5 for FT Tau, DK Tau B, and IRAS 04370+2559; M3.5–M6 for IRAS 04200+2759, IT Tau B, and ITG 1; and M6–M8 for IRAS 04325+2402 C. In addition, the values of K_s − [3.6] in Table 13 and Figure 26 for spectral types of M4–M9 are incorrect. We present corrected versions of Table 13 and Figure 26.

**Figure 26.** Infrared colors as a function of spectral type for members of the Taurus and Chamaeleon I star-forming regions (small filled circles) and young sources in the η Cha, Cha, and TW Hya associations and in the solar neighborhood (large filled circles). The latter samples should have negligible extinction (*A_V* < 1). We have used these data to estimate the intrinsic colors of young stellar photospheres (solid lines, Table 13). Because few young late-type objects have been measured at 24 μm, we also show data for field dwarfs at M9–L0 in the diagram of [8.0] − [24] colors (open circles).
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epsilon — **Figure 26.** Infrared colors as a function of spectral type for members of the Taurus and Chamaeleon I star-forming regions (small filled circles) and young sources in the η Cha, Cha, and TW Hya associations and in the solar neighborhood (large filled circles). The latter samples should have negligible extinction (*A_V* < 1). We have used these data to estimate the intrinsic colors of young stellar photospheres (solid lines, Table 13). Because few young late-type objects have been measured at 24 μm, we also show data for field dwarfs at M9–L0 in the diagram of [8.0] − [24] colors (open circles).
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Table 13. Colors of Young Stellar Photospheres

Spectral Type	J − H	H − K_s	K_s − [3.6]	[3.6] − [4.5]	[4.5] − [5.8]	[5.8] − [8.0]	[8.0] − [24]
K4	0.53	0.10	0.06	0.00	0.04	0.00	0.04
K5	0.61	0.12	0.08	0.00	0.04	0.00	0.06
K6	0.66	0.14	0.10	0.00	0.04	0.00	0.08
K7	0.68	0.15	0.10	0.00	0.04	0.00	0.11
M0	0.70	0.16	0.10	0.00	0.04	0.00	0.13
M1	0.71	0.18	0.11	0.01	0.04	0.00	0.15
M2	0.70	0.20	0.14	0.03	0.04	0.00	0.17
M3	0.68	0.22	0.17	0.05	0.04	0.00	0.19
M4	0.63	0.26	0.20	0.07	0.04	0.00	0.21
M5	0.56	0.29	0.28	0.09	0.04	0.00	0.23
M6	0.55	0.33	0.39	0.11	0.04	0.00	0.25
M7	0.59	0.37	0.42	0.12	0.05	0.00	0.27
M8	0.65	0.44	0.52	0.12	0.07	0.03	0.29
M9	0.72	0.55	0.63	0.14	0.13	0.12	0.31
L0	0.98	0.66	0.72	0.16	0.22	0.25	0.33

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