2004ApJ...600..435M


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.21CEST13:15:22

2004ApJ...600..435M - Astrophys. J., 600, 435-450 (2004/January-1)

Ten micron observations of nearby young stars.

METCHEV S.A., HILLENBRAND L.A. and MEYER M.R.

Abstract (from CDS):

We present new 10 µm photometry of 21 nearby young stars obtained at the Palomar 5 m and at the Keck I 10 m telescopes as part of a program to search for dust in the habitable zone of young stars. Thirteen of the stars are in the F-K spectral type range (``solar analogs''), four have B or A spectral types, and four have spectral type M. We confirm existing IRAS 12 µm and ground-based 10 µm photometry for 10 of the stars and present new insight into this spectral regime for the rest. Excess emission at 10 µm is not found in any of the young solar analogs, except for a possible 2.4 σ detection in the G5 V star HD 88638. The G2 V star HD 107146, which does not display a 10 µm excess, is identified as a new Vega-like candidate, based on our 10 µm photospheric detection, combined with previously unidentified 60 and 100 µm IRAS excesses. Among the early-type stars, a 10 µm excess is detected only in HD 109573A (HR 4796A), confirming prior observations; among the M dwarfs, excesses are confirmed in AA Tau, CD -40°8434, and Hen 3-600A. A previously suggested N-band excess in the M3 dwarf CD -33°7795 is shown to be consistent with photospheric emission. We calculate infrared to stellar bolometric luminosity ratios for all stars exhibiting mid-infrared excesses and infer the total mass of orbiting dust in the cases of optically thin disks. For a derived median photometric precision of ±0.11 mag, we place an upper limit of Mdust~2x10–5 Mon the dust mass (assuming a dust temperature of 300 K) around solar analogs not seen in excess at 10 µm. Our calculations for the nearby K1 V star HD 17925 show that it may have the least massive debris disk known outside our solar system (Mdust≳7x10–6 M). Our limited data confirm the expected tendency of decreasing fractional dust excess fd=LIR/L* with increasing stellar age. However, we argue that estimates of f_d_suffer from a degeneracy between the temperature and the amount of circumstellar dust Mdust, and we propose a relation of Mdustas a function of age instead.

Abstract Copyright:

Journal keyword(s): Stars: Circumstellar Matter - ISM: Dust, Extinction - Infrared: Stars - Stars: Planetary Systems: Protoplanetary Disks

Simbad objects: 32

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Number of rows : 32

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 * bet And PM* 01 09 43.92388 +35 37 14.0075 5.58 3.62 2.05 0.81 -0.19 M0+IIIa 529 0
2 BD+17 232 ** 01 37 39.3898708 +18 35 32.700834   11.610 9.830 9.39 8.381 G/K 47 0
3 HD 17925 RS* 02 52 32.1281853696 -12 46 10.970649463 7.48 6.91 6.05 5.34 4.89 K1V 457 0
4 V* V525 Per BY* 03 19 02.7581136374 +48 10 59.613783798   12.92       ~ 22 0
5 * alf Per V* 03 24 19.3700924 +49 51 40.245455 2.64 2.27 1.79     F5Ib 791 2
6 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1658 1
7 V* DH Tau TT* 04 29 41.558 +26 32 58.27 15.14 14.62 13.10 13.01   M1Ve 255 1
8 V* DI Tau TT* 04 29 42.4736177473 +26 32 49.119618729 16.39 15.20 13.60     M0Ve 188 0
9 V* AA Tau TT* 04 34 55.4222683130 +24 28 53.038273587 13.14 13.34 12.20     K5Ve 599 0
10 * zet Lep * 05 46 57.3409587 -14 49 19.019943   3.637 3.525     A2IV-V(n) 277 0
11 HD 60737 PM* 07 38 16.4409933710 +47 44 55.221629265       7.3   G0 41 0
12 * bet Gem PM* 07 45 18.94987 +28 01 34.3160 3.00 2.14 1.14 0.39 -0.11 K0IIIb 1036 1
13 V* V478 Hya BY* 08 22 49.9528448767 +01 51 33.554224835   9.30 8.711   7.999 G1/2V 84 2
14 BD+45 1575a PM* 08 24 13.2265547707 +44 56 45.328463384   10.09   8.6   K2V 29 1
15 HD 70516 PM* 08 24 15.6562755632 +44 56 58.960185580   8.31   7.3   G2V 61 1
16 HD 77407 ** 09 03 27.0836286593 +37 50 27.500788701       6.7   G0V+M3V-M6V 86 0
17 V* LX UMa BY* 10 14 35.7866400432 +53 46 15.161029033       7.6   G5 33 0
18 NAME TW Hya Association As* 11 01.9 -34 42           ~ 795 0
19 CD-38 6968 PM* 11 09 40.0907909831 -39 06 47.280172529   10.52 9.93     G3 8 0
20 Hen 3-600 TT* 11 10 27.894 -37 31 51.97   13.53 12.05 11.61 9.29 M4Ve+M4Ve 195 0
21 TWA 3A TT* 11 10 28.00 -37 31 51.0   14.04 12.57   9.10 M4Ve 181 0
22 CD-33 7795 TT* 11 31 55.2603055856 -34 36 27.214242128   12.97 11.524 11.150 9.150 M2Ve 165 0
23 * bet Leo dS* 11 49 03.57834 +14 34 19.4090 2.30 2.22 2.13 2.08 2.06 A3Va 533 0
24 HD 107146 PM* 12 19 06.5022221429 +16 32 53.870713669   7.61   6.7   G2V 211 0
25 HD 109573 PM* 12 36 01.0317721349 -39 52 10.222698506   5.786 5.774 7.25 5.81 A0V 535 1
26 V* V1032 Cen TT* 14 08 10.1545137760 -41 23 52.576649494     12.199   10.506 K7IVe 68 0
27 * alf Boo RG* 14 15 39.67207 +19 10 56.6730 2.46 1.18 -0.05 -1.03 -1.68 K1.5IIIFe-0.5 2090 0
28 NAME Upper Sco Association As* 16 12 -23.4           ~ 959 1
29 HD 145519 SB* 16 12 05.9977976148 -19 03 44.399370363   8.19 8.00     B9V 36 0
30 HD 147809 ** 16 24 59.1476819338 -25 21 17.984250932   8.99 8.63     A1V 46 0
31 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2472 0
32 V* TW PsA BY* 22 56 24.0532946025 -31 33 56.035064606   7.58 6.48     K4Ve 263 0

    Equat.    Gal    SGal    Ecl

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2019.10.21-13:15:22

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