2006A&A...459..545G


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.10CET20:08:56

2006A&A...459..545G - Astronomy and Astrophysics, volume 459, 545-556 (2006/11-4)

C2D Spitzer-IRS spectra of disks around T Tauri stars. II. PAH emission features.

GEERS V.C., AUGEREAU J.-C., PONTOPPIDAN K.M., DULLEMOND C.P., VISSER R., KESSLER-SILACCI J.E., EVANS II N.J., VAN DISHOECK E.F., BLAKE G.A., BOOGERT A.C.A., BROWN J.M., LAHUIS F. and MERIN B.

Abstract (from CDS):

We search for Polycyclic Aromatic Hydrocarbon (PAH) features towards young low-mass (T Tauri) stars and compare them with surveys of intermediate mass (Herbig Ae/Be) stars. The presence and strength of the PAH features are interpreted with disk radiative transfer models exploring the PAH feature dependence on the incident UV radiation, PAH abundance and disk parameters. Spitzer Space Telescope 5-35µm spectra of 54 pre-main sequence stars with disks were obtained, consisting of 38 T Tauri, 7 Herbig Ae/Be and 9 stars with unknown spectral type. Compact PAH emission is detected towards at least 8 sources of which 5 are Herbig Ae/Be stars. The 11.2µm PAH feature is detected in all of these sources, as is the 6.2µm PAH feature for the 4 sources for which short wavelength data are available. However, the 7.7 and 8.6µm features appear strongly in only 1 of these 4 sources. Based on the 11.2µm feature, PAH emission is observed towards at least 3 T Tauri stars, with 14 tentative detections, resulting in a lower limit to the PAH detection rate of 8%. The lowest mass source with PAH emission in our sample is T Cha with a spectral type G8. All 4 sources in our sample with evidence for dust holes in their inner disk show PAH emission, increasing the feature/continuum ratio. Typical 11.2µm line intensities are an order of magnitude lower than those observed for the more massive Herbig Ae/Be stars. Measured line fluxes indicate PAH abundances that are factors of 10-100 lower than standard interstellar values. Conversely, PAH features from disks exposed to stars with Teff≤4200K without enhanced UV are predicted to be below the current detection limit, even for high PAH abundances. Disk modeling shows that the 6.2 and 11.2µm features are the best PAH tracers for T Tauri stars, whereas the 7.7 and 8.6µm bands have low feature over continuum ratios due to the strongly rising silicate emission.

Abstract Copyright:

Journal keyword(s): stars: pre-main sequence - planetary systems: protoplanetary disks - circumstellar matter - astrochemistry - ISM: molecules

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 - 2020
#notes
1 NAME LDN 1455 IRS 2 cor 03 27 47.6826386762 +30 12 04.459144041     19.6     ~ 93 1
2 EM* LkHA 330 TT* 03 45 48.2804487421 +32 24 11.851014679   12.30 10.97     F7 116 0
3 IRAS 03446+3254 FIR 03 47 47.35 +33 04 01.2           ~ 20 0
4 V* V710 Tau Or* 04 31 57.797 +18 21 35.06           M2/3e+M0.5/1e 140 0
5 V* DM Tau TT* 04 33 48.7335659850 +18 10 09.974471722 14.30 14.82 14.00     M2Ve 491 0
6 NAME Taurus Dark Cloud SFR 04 41.0 +25 52           ~ 3335 0
7 CoKu Tau-Aur Star 4 TT* 04 41 16.8106225314 +28 40 00.077173462   16.40 14.68 14.59   M1.5e 165 0
8 V* GM Aur TT* 04 55 10.9813656049 +30 21 59.375978047 14.59 14.22 13.10     K3Ve 533 0
9 V* V1366 Ori EB* 05 16 00.4764811920 -09 48 35.394685295 10.19 10.16 9.84 9.77 9.63 B9.5V 159 0
10 V* RR Tau Ae* 05 39 30.5114685049 +26 22 26.961204895 11.64 12.09 11.28 10.58 10.17 A0:IVe 216 0
11 V* SX Cha Or* 10 55 59.731 -77 24 39.91   15.88 16.71   12.35 M1.5+M3 79 0
12 V* SY Cha Or* 10 56 30.3882538728 -77 11 39.402450501         11.29 K5Ve 111 0
13 V* VW Cha TT* 11 08 01.3974165580 -77 42 28.579297348 13.91 14.04 12.80   10.69 K7+M0 166 0
14 V* VZ Cha Or* 11 09 23.7736314968 -76 23 20.855918834   13.82 12.94   12.14 K7e 122 0
15 V* WX Cha Or* 11 09 58.738 -77 37 08.88   16.44 13.70   12.20 M1+M5 89 0
16 HD 98922 Be* 11 22 31.6740564115 -53 22 11.456030308   6.80 6.76     B9Ve 111 1
17 HD 101412 Be* 11 39 44.4562795603 -60 10 27.717502041   9.465 9.288     A3VaekA0mA0_lB 111 0
18 V* T Cha Or* 11 57 13.5268556629 -79 21 31.521755129   10.00 11.86     K0e 225 1
19 V* DL Cha LP* 13 06 08.3990620091 -77 06 27.214812252   12.79 11.57     M6III 22 0
20 CPD-36 6759 Y*O 15 15 48.4459023859 -37 09 16.026315179   9.21 8.708     F8V 332 1
21 HD 135344 * 15 15 48.9457954324 -37 08 55.727525343   7.84 7.76     A0V 126 1
22 CD-33 10685 TT* 15 45 12.8670160092 -34 17 30.646921079 12.47 11.56 10.224 9.60 8.685 K3Ve 210 1
23 V* GW Lup TT* 15 46 44.7292759994 -34 30 35.677245389   13.8       M1.5e 77 0
24 THA 15-5 TT* 15 47 56.9433443193 -35 14 34.797849332   14.5 16.2     K7e 60 0
25 HD 141569 pr* 15 49 57.7484743862 -03 55 16.344023102 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 454 0
26 HD 142666 TT* 15 56 40.0222941557 -22 01 40.004849949 9.41 9.37 8.82 8.31 8.01 F0V_sh 204 0
27 V* RU Lup TT* 15 56 42.3109948086 -37 49 15.473469159 9.27 10.07 9.60     K7/M0e 371 0
28 Sz 84 TT* 15 58 02.5212129160 -37 36 02.733294310   14.3       M5.0e 49 0
29 HD 144432 Ae* 16 06 57.9530266912 -27 43 09.758016578 8.47 8.53 8.19 7.82 7.53 A9/F0V 207 1
30 WRAY 16-203 TT* 16 08 29.7086692265 -39 03 10.994386198   16.26 15.91 15.38 15.69 K0: 149 1
31 Elia 2-20 TT* 16 26 18.8782824640 -24 28 19.698059817           ~ 88 1
32 GSS 31 TT* 16 26 23.3694945462 -24 20 59.580653864   15.9 14.70 14.33 11.53 K0e 131 1
33 GSS 32 TT* 16 26 24.0521249616 -24 24 48.105099750       17.81 15.58 K5-K6 93 1
34 EM* SR 21A TT* 16 27 10.2776332501 -24 19 12.620553212   16.08 14.10     G1 225 1
35 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 2944 0
36 Haro 1-17 Y*O 16 32 21.9312543188 -24 42 14.835977855   16.76 15.61     M2.5e 35 0
37 HBC 650 TT* 16 34 29.32 -15 47 01.4           K3.0 164 2
38 CPD-56 8032 PN 17 09 00.86008 -56 54 48.0957 11.24 11.48 11.04     [WC10] 245 0
39 HD 163296 Ae* 17 56 21.2882188601 -21 57 21.872343282 7.00 6.93 6.85 6.86 6.67 A1Vep 738 0
40 HD 169142 Ae* 18 24 29.7799676975 -29 46 49.328597698   8.42 8.16     F1VekA3mA3_lB? 306 2
41 V* VV Ser Ae* 18 28 47.8619658319 +00 08 39.924642619 12.99 12.63 11.80 11.01 10.24 A5Ve 225 0
42 2MASS J18295433+0115017 Y*O 18 29 54.34 +01 15 01.8           ~ 10 0
43 HBC 672 Em* 18 29 56.8828626544 +01 14 46.339137067   17.6       K8.0 98 0
44 2MASS J18295760+0113004 Y*O 18 29 57.602 +01 13 00.42           ~ 34 3
45 IRAS 18274+0112 Y*O 18 29 57.73680 +01 14 05.6940           M4: 132 2
46 [EC92] 95 Y*O 18 29 57.893 +01 12 46.25           K1.0 71 3
47 2MASS J18295820+0115216 Y*O 18 29 58.2037104611 +01 15 21.603460135           K7.0 37 0
48 HD 179218 Ae* 19 11 11.2540715594 +15 47 15.632212730 7.55 7.476 7.39 7.25 7.21 A0Ve 213 0
49 [D75b] Em* 21-021 PN 21 29 58.4712776885 +51 04 00.323547316   15.66 14.20 13.89   O7(f)/[WC11] 224 0

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2019.12.10-20:08:56

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