2003ApJ...594..279G


Query : 2003ApJ...594..279G

2003ApJ...594..279G - Astrophys. J., 594, 279-293 (2003/September-1)

A quantitative comparison of the Small Magellanic Cloud, Large Magellanic Cloud, and Milky Way ultraviolet to near-infrared extinction curves.

GORDON K.D., CLAYTON G.C., MISSELT K.A., LANDOLT A.U. and WOLFF M.J.

Abstract (from CDS):

We present an exhaustive quantitative comparison of all the known extinction curves in the Small and Large Magellanic Clouds (SMC and LMC) with our understanding of the general behavior of Milky Way extinction curves. The RV-dependent CCM relationship of Cardelli, Clayton, and Mathis and the sample of extinction curves used to derive this relationship are used to describe the general behavior of Milky Way extinction curves. The ultraviolet portion of the SMC and LMC extinction curves are derived from archival IUE data, except for one new SMC extinction curve, which was measured using Hubble Space Telescope Space Telescope Imaging Spectrograph observations. The optical extinction curves are derived from new (for the SMC) and literature UBVRI photometry (for the LMC). The near-infrared extinction curves are calculated mainly from 2MASS photometry supplemented with DENIS and new JHK photometry. For each extinction curve, we give RV=A(V)/E(B-V) and N(H I) values that probe the same dust column as the extinction curve. We compare the properties of the SMC and LMC extinction curves with the CCM relationship three different ways: each curve by itself, the behavior of extinction at different wavelengths with RV, and the behavior of the extinction curve Fitzpatrick and Massa fit parameters with RV. As has been found previously, we find that a small number of LMC extinction curves are consistent with the CCM relationship, but the majority of the LMC and all the SMC curves do not follow the CCM relationship. For the first time, we find that the CCM relationship seems to form a bound on the properties of all the LMC and SMC extinction curves. This result strengthens the picture dust extinction curves exhibit of a continuum of properties between those found in the Milky Way and the SMC bar. Tentative evidence based on the behavior of the extinction curves with dust-to-gas ratio suggests that the continuum of dust extinction curves is possibly caused by the environmental stresses of nearby star formation activity.

Abstract Copyright: ∼

Journal keyword(s): ISM: Dust, Extinction - Galaxies: ISM - Galaxies: Magellanic Clouds - Ultraviolet: ISM

Simbad objects: 49

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Number of rows : 49
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 SK 13 s*b 00 47 12.2164410744 -73 06 33.111710784   12.52 12.48     B1.5Ia 83 0
2 SK 17 s*b 00 47 38.9029190112 -73 22 53.855881572 11.563 12.324 12.236     B3Ia 39 0
3 SK 35 s*b 00 50 18.1229621664 -72 38 10.034313252 11.04 10.96 12.40   12.12 O9.5Iab 48 0
4 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 12317 1
5 AzV 214 s*b 00 58 54.7802134728 -72 13 17.172789780   13.40 13.39     B1Ia 38 0
6 SK 103 s*b 01 01 58.7783887824 -72 35 38.956138008 11.233 12.284 12.396   12.46 B0Ia 33 0
7 SK 120 s*b 01 05 24.7610544984 -73 03 52.973560260 12.47 13.43 13.53   13.56 B1-1.5I 27 1
8 AzV 398 s*b 01 06 09.8134902360 -71 56 00.746371284 13.15 13.94 13.98   13.71 O9.7Ia 48 0
9 SK 128 s*b 01 06 29.2604555136 -72 22 08.607372996   11.7 11.8     B2.5Ia 32 0
10 SK 143 s*b 01 10 55.7567270880 -72 42 56.223094032 12.15 12.98 12.89 12.78 11.64 O9.7Ib 91 0
11 SK 145 s*b 01 11 25.9167352608 -72 31 21.276515892 11.463 12.464 12.596   11.60 B2.5Ia 42 0
12 HD 270754 s*b 04 47 04.4509965192 -67 06 53.121123648 10.351 11.219 11.26   10.992 B1.5Ia 92 0
13 HD 268605 s*b 04 50 18.9258130824 -67 39 38.036838240 10.244 11.2 11.377   11.322 O9.5/B0Ia 99 0
14 SK -66 19 * 04 55 53.951 -66 24 59.35   14.98 14.87     O7V 27 0
15 HD 268732 s*b 04 57 04.4395141656 -66 34 38.571040380 10.652 11.494 11.587     BC1Iab 60 0
16 SK -65 15 * 04 59 41.3682114672 -65 49 50.002616640 11.288 12.11 12.02   12.312 OB 18 0
17 SK -68 23 * 05 00 49.4717504928 -68 07 09.733713888   13.03 12.81     OB 14 0
18 CPD-67 381 Pu* 05 01 22.5825475560 -67 20 09.986762652 11.042 11.93 12.42   12.024 OB 15 0
19 SK -68 26 s*b 05 01 32.2453117296 -68 10 42.937181508 10.822 11.728 11.85     BC2Ia 41 0
20 CPD-68 312 * 05 05 15.1972545600 -68 02 14.146413504 10.810 11.721 11.71   11.725 OB 27 0
21 SK -68 41 * 05 05 27.1146438696 -68 10 02.642123460 10.855 11.868 12.01   12.086 B0.7Ia 59 0
22 HD 269392 * 05 19 51.8115702216 -69 53 08.524603608   12.36 12.12 11.87   B3I 40 0
23 HD 269371 * 05 20 19.0830107928 -67 18 05.679651096   11.3 11.0     B3Ia 54 0
24 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 19090 0
25 SK -66 88 * 05 25 37.2300651408 -66 14 29.278811328   12.90 12.70     OB 12 0
26 HD 269504 Pu* 05 25 38.9263896528 -67 19 00.061068936   11.86 11.95     OB 32 0
27 HD 271294 * 05 28 39.4513417632 -65 39 00.631527804 11.919 12.40 12.56   12.240 OB 21 0
28 SK -66 106 * 05 29 00.9965765448 -66 38 27.790072368   12.64 12.72     OB 19 0
29 SK -66 118 * 05 30 51.9088749432 -66 54 09.081058104 11.075 11.47 11.28     OB 22 0
30 HD 269702 s*b 05 31 52.1192227056 -67 34 20.768696508   11.69 11.99     O8I(f)p 35 0
31 SK -69 206 * 05 35 35.9718223824 -69 07 06.552258708   12.99 12.82 12.99   OB 12 0
32 W61 27-27 * 05 36 03.7921076496 -69 01 30.109967868 12.313 13.004 12.706 12.42 10.428 B1.5I 18 0
33 CPD-69 416 s*b 05 36 17.0922496704 -69 11 03.678516168   12.15 12.16     BC1Ia 35 0
34 W61 27-56 s*b 05 36 26.7746241720 -68 57 32.036561136 11.973 12.864 12.836   11.827 B1I 32 0
35 SK -66 169 s*b 05 36 54.6614083464 -66 38 22.427577744   12.43 12.56     O9.7Ia+ 37 0
36 CPD-69 436 s*b 05 37 09.1787926949 -69 20 19.505185054   12.182 12.139 12.338   BC1.5Ia 32 0
37 HD 269900 * 05 37 41.0147529864 -67 43 16.568563296 8.716 11.44 11.475   9.800 OB 31 0
38 NAME 30 Dor Nebula SFR 05 38 36.0 -69 05 11           ~ 1276 2
39 SK -68 140 s*b 05 38 57.1713887928 -68 56 53.151615708   12.81 12.71 12.89   B0.7Ib-IabNwk 53 0
40 SK -69 256 s*b 05 39 55.7304859200 -69 16 25.889831940 11.713 12.644 12.666   12.772 B1Iab 17 0
41 CPD-69 491 * 05 40 48.8049243960 -69 16 51.205287720   12.00 11.88     B3I 18 0
42 HD 269997 s*b 05 41 20.3933761824 -69 05 07.273296276   11.36 11.20     B2.5Ia 62 0
43 NAME LMC 2 Supergiant Shell sh 05 41 27 -69 22.4           ~ 200 0
44 SK -69 279 s*b 05 41 44.6553703752 -69 35 14.905767516 12.079 12.787 12.842 13.03 12.619 ON9.5Ia+ 70 0
45 SK -69 280 * 05 41 48.9396288888 -69 17 52.388147364   12.66 12.66     OB 17 0
46 SK -68 155 s*b 05 42 54.9424084824 -68 56 54.480574752   12.75 12.72     O9Ia 37 0
47 CPD-67 500 Em* 05 44 25.0227763560 -67 13 49.579736268 10.857 11.76 11.751 12.13 11.857 OB 29 0
48 HD 270151 s*b 05 49 02.8404797232 -70 02 30.130973592 11.141 12.174 12.02   11.655 B2Ia 42 0
49 HD 270196 s*b 05 51 20.7793116768 -70 17 09.299979960 10.038 11.490 11.6   11.646 B1.5Ia 59 0

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