2004ApJ...600..435M


Query : 2004ApJ...600..435M

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 M⊕on 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 - 2026
#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 572 1
2 BD+17 232 ** 01 37 39.409920 +18 35 33.25920   11.062 9.891 9.386 8.381 K7e 58 0
3 HD 17925 RS* 02 52 32.1281856011 -12 46 10.968056223 7.48 6.91 6.05 5.34 4.89 K1V 557 0
4 V* V525 Per BY* 03 19 02.7579384576 +48 10 59.576839464   12.92       ~ 29 0
5 * alf Per V* 03 24 19.3700924 +49 51 40.245455 2.64 2.27 1.79     F5Ib 870 1
6 * eps Eri BY* 03 32 55.8444911587 -09 27 29.739493865 5.19 4.61 3.73 3.00 2.54 K2V 2073 1
7 V* DH Tau Or* 04 29 41.5525353432 +26 32 58.126559604 15.14 14.62 13.10 13.01   M1Ve 323 0
8 V* DI Tau Or* 04 29 42.4723379736 +26 32 49.128692676 16.39 15.20 13.60     M0Ve 223 0
9 V* AA Tau Or* 04 34 55.4201902392 +24 28 53.033624580 13.14 13.34 12.20 12.03   K5Ve 801 0
10 * zet Lep * 05 46 57.3413646658 -14 49 19.020570470   3.637 3.525     A2IV-V(n) 308 0
11 HD 60737 PM* 07 38 16.4410103088 +47 44 55.220375940       7.3   G0 60 0
12 * bet Gem PM* 07 45 18.94987 +28 01 34.3160 3.00 2.14 1.14 0.39 -0.11 K0IIIb 1150 2
13 V* V478 Hya BY* 08 22 49.9527726648 +01 51 33.552251064   9.30 8.711   7.999 G1/2V 112 2
14 BD+45 1575a PM* 08 24 13.2262375704 +44 56 45.325404096   10.09   8.6   K2V 46 1
15 HD 70516 PM* 08 24 15.6561750264 +44 56 58.956488592   8.31   7.3   G2V 88 1
16 HD 77407 PM* 09 03 27.0837288552 +37 50 27.493558584   7.63 7.04     G0V 110 0
17 V* LX UMa BY* 10 14 35.7684378000 +53 46 15.013753752       7.6   G5 46 0
18 NAME TW Hya Association As* 11 01.9 -34 42           ~ 1018 0
19 CD-38 6968 PM* 11 09 40.0907929752 -39 06 47.281570596   10.52 9.93     G3 12 0
20 TWA 3 ** 11 10 27.894072 -37 31 51.96612   13.53 12.05 11.61 9.29 M4Ve+M4Ve 218 0
21 TWA 3A TT* 11 10 27.9121410480 -37 31 51.535547940   14.04 12.57   9.10 M4Ve 221 0
22 CD-33 7795 TT* 11 31 55.2608963280 -34 36 27.203892120   12.97 11.524 11.150 9.150 M2Ve 205 0
23 * bet Leo dS* 11 49 03.57834 +14 34 19.4090 2.30 2.22 2.13 2.08 2.06 A3Va 605 1
24 HD 107146 PM* 12 19 06.5018840304 +16 32 53.867731128   7.61   6.7   G2V 307 0
25 HD 109573 TT* 12 36 01.0317461592 -39 52 10.220465388   5.786 5.774   5.81 A0V 684 1
26 CD-40 8434 TT* 14 08 10.1545500744 -41 23 52.573291080   13.42 12.18 11.71 10.506 K7IVe 546 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 2417 1
28 NAME Upper Sco Association As* 16 12 -23.4           ~ 1586 1
29 HD 145519 SB* 16 12 05.9979800304 -19 03 44.400646836   8.19 8.00   7.44 B9V 53 0
30 HD 147809 ** 16 24 59.1476326440 -25 21 17.974751148   9.02 8.62     A1V 68 0
31 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0V 2787 1
32 V* TW PsA BY* 22 56 24.0525564918 -31 33 56.030584767   7.58 6.48     K4Ve 316 0

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