2005ApJ...629..512U


Query : 2005ApJ...629..512U

2005ApJ...629..512U - Astrophys. J., 629, 512-525 (2005/August-2)

Identification of main-sequence stars with mid-infrared excesses using GLIMPSE: β Pictoris analogs?

UZPEN B., KOBULNICKY H.A., OLSEN K.A.G., CLEMENS D.P., LAURANCE T.L., MEADE M.R., BABLER B.L., INDEBETOUW R., WHITNEY B.A., WATSON C., WOLFIRE M.G., WOLFF M.J., BENJAMIN R.A., BANIA T.M., COHEN M., DEVINE K.E., DICKEY J.M., HEITSCH F., JACKSON J.M., MARSTON A.P., MATHIS J.S., MERCER E.P., STAUFFER J.R., STOLOVY S.R., BACKMAN D.E. and CHURCHWELL E.

Abstract (from CDS):

Spitzer IRAC 3.6-8 µm photometry obtained as part of the GLIMPSE survey has revealed mid-infrared excesses for 33 field stars with known spectral types in a 1.2 deg2 field centered on the southern Galactic H II region RCW 49. These stars comprise a subset of 184 stars with known spectral classification, most of which were preselected to have unusually red IR colors. We propose that the mid-IR excesses are caused by circumstellar dust disks that are either very late remnants of stellar formation or debris disks generated by planet formation. Of these 33 stars, 29 appear to be main-sequence stars on the basis of optical spectral classifications. Five of the 29 main-sequence stars are O or B stars with excesses that can be plausibly explained by thermal bremsstrahlung emission, and four are post-main-sequence stars. The lone O star is an O4 V((f)) at a spectrophotometric distance of 3233+540–535 pc and may be the earliest member of the Westerlund 2 cluster. Of the remaining 24 main-sequence stars, 18 have spectral energy distributions that are consistent with hot dusty debris disks, a possible signature of planet formation. Modeling the excesses as blackbodies demonstrates that the blackbody components have fractional bolometric disk-to-star luminosity ratios, LIR/L*, ranging from 10–3 to 10–2 with temperatures ranging from 220 to 820 K. The inferred temperatures are more consistent with asteroid belts than with the cooler temperatures expected for Kuiper belts. Mid-IR excesses are found in all spectral types from late B to early K.

Abstract Copyright:

Journal keyword(s): Stars: Circumstellar Matter - Galaxy: Open Clusters and Associations: Individual: Alphanumeric: Westerlund 2 - Stars: Planetary Systems: Formation

Nomenclature: Tables 1, 2: [UKO2005] NN (Nos 1-33).

Simbad objects: 40

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Number of rows : 40
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 * eps Eri BY* 03 32 55.8444911587 -09 27 29.739493865 5.19 4.61 3.73 3.00 2.54 K2V 1837 1
2 * zet Lep * 05 46 57.3409587 -14 49 19.019943   3.637 3.525     A2IV-V(n) 291 0
3 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1813 1
4 2MASS J10210640-5743271 * 10 21 06.4001173368 -57 43 27.174245772           F5IV/V 1 0
5 2MASS J10212181-5739183 * 10 21 21.8091926184 -57 39 18.400905972           F3V 1 0
6 2MASS J10212249-5746404 * 10 21 22.5010895064 -57 46 40.574483616           G2V 1 0
7 2MASS J10213333-5735398 * 10 21 33.3413251008 -57 35 39.859879416           K5V 1 0
8 LLNS 929 * 10 21 33.7871768904 -57 33 22.912496856   11.90 11.82     B9V 3 0
9 2MASS J10214145-5750415 * 10 21 41.4572627544 -57 50 41.509442616           B8V 1 0
10 TYC 8608-2031-1 * 10 21 54.6298017000 -57 39 21.840571044   12.38 12.41     B8V 1 0
11 2MASS J10220574-5753460 * 10 22 05.7469694256 -57 53 46.009214196           B5V 4 0
12 TYC 8608-808-1 * 10 22 12.4405836264 -57 31 32.497779504   10.52 10.41     B2V 2 0
13 2MASS J10221550-5727151 * 10 22 15.4908237960 -57 27 15.166645848           G8IV 1 0
14 2MASS J10224039-5751461 * 10 22 40.3818054696 -57 51 46.195129188           A2V 1 0
15 2MASS J10224485-5738431 * 10 22 44.8530150912 -57 38 43.116923940           G0V 1 0
16 2MASS J10224911-5729455 * 10 22 49.1156741448 -57 29 45.613855716           G5V 1 0
17 2MASS J10225509-5721302 * 10 22 55.0995177264 -57 21 30.236235696           G0V 1 0
18 2MASS J10225656-5726168 * 10 22 56.5693788600 -57 26 16.831855824           A7V 1 0
19 2MASS J10225795-5734130 * 10 22 57.9440994648 -57 34 13.071957600           G8II 1 0
20 2MASS J10230066-5731474 * 10 23 00.6495852792 -57 31 47.517662604           F5II 1 0
21 2MASS J10230188-5729511 * 10 23 01.8762500352 -57 29 51.145096380           K0V 1 0
22 HD 90187 Be* 10 23 07.8387872352 -57 59 51.216413604 8.16 8.95 8.65 9.41   B0/3e(p) 42 0
23 2MASS J10230932-5727250 * 10 23 09.3233116128 -57 27 25.089433812           F8V 1 0
24 2MASS J10231333-5726356 * 10 23 13.3360897296 -57 26 35.618398152           F5IV 1 0
25 2MASS J10231576-5730119 * 10 23 15.7616911680 -57 30 11.918276244           K5V 1 0
26 2MASS J10232601-5730435 * 10 23 26.0085226224 -57 30 43.474758336           F3IV 1 0
27 HD 302747 * 10 23 26.7371547576 -57 36 24.925622148   11.81 11.77     A7V 3 0
28 2MASS J10235162-5712213 * 10 23 51.6244928592 -57 12 21.365760024           G8III 1 0
29 CD-56 3323 Em* 10 23 54.5104516824 -57 36 00.481763340   11.1 11.1     B1V(e) 7 0
30 Cl Westerlund 2 OpC 10 23 58.1 -57 45 49           ~ 329 0
31 Cl Westerlund 2 5 * 10 24 02.4404730984 -57 44 36.147162768 14.149 14.514 13.155 12.2   O5/5.5V/III(f) 26 0
32 2MASS J10241078-5710353 * 10 24 10.7918364648 -57 10 35.333178960           F5II 1 0
33 GUM 29 HII 10 24 14.6 -57 46 58           ~ 204 0
34 WR 20b WR* 10 24 18.3978418584 -57 48 29.776921704     13.7 12.0   WN6ha 54 0
35 2MASS J10242577-5736016 * 10 24 25.7692023264 -57 36 01.691848008           A5V 1 0
36 2MASS J10245840-5741272 Y*? 10 24 58.406 -57 41 27.27 17.876 20.186 17.931   15.148 F8Ve 2 0
37 TYC 8608-10-1 * 10 25 03.5850961728 -57 41 40.997677020   11.89 11.83     A3V 3 0
38 2MASS J10253880-5747417 * 10 25 38.7959225760 -57 47 41.704347588           A7V 1 0
39 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2623 0
40 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1195 3

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2023.01.27-14:35:49

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