2013A&A...549A..92G


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST01:02:30

2013A&A...549A..92G - Astronomy and Astrophysics, volume 549A, 92-92 (2013/1-1)

A sensitive survey for 13CO, CN, H2CO, and SO in the disks of T Tauri and Herbig Ae stars.

GUILLOTEAU S., DI FOLCO E., DUTREY A., SIMON M., GROSSO N. and PIETU V.

Abstract (from CDS):

We investigate the suitability of several molecular tracers, in particular CN N=2-1 line emission, as a confusion-free probe of the kinematics of circumstellar disks. We use the IRAM 30-m telescope to perform a sensitive search for CN N=2-1 in 42 T Tauri or Herbig Ae systems located principally in the Taurus-Auriga region. 13CO J=2-1 is observed simultaneously to provide an indication of the level of confusion with the surrounding molecular cloud. The bandpass also contains two transitions of ortho-H2CO, one of SO and the C17O J=2-1 line which provide complementary information on the nature of the emission. While 13CO is in general dominated by residual emission from the cloud, CN exhibits a high disk detection rate >50% in our sample. We even report CN detection in stars for which interferometric searches failed to detect 12CO, presumably because of obscuration by a foreground, optically thick, cloud. Comparison between CN and o-H2CO or SO line profiles and intensities divide the sample in two main categories. Sources with SO emission are bright and have strong H2CO emission, leading in general to [H2CO/CN]>0.5. Furthermore, their line profiles, combined with a priori information on the objects, suggest that the emission is coming from outflows or envelopes rather than from a circumstellar disk. On the other hand, most sources have [H2CO/CN]<0.3, no SO emission, and some of them exhibit clear double-peaked profiles characteristics of rotating disks. In this second category, CN is likely tracing the proto-planetary disks. From the line flux and opacity derived from the hyperfine ratios, we constrain the outer radii of the disks, which range from 300 to 600 AU. The overall gas disk detection rate (including all molecular tracers) is ∼68 %, and decreases for fainter continuum sources. The current study demonstrates that gas disks, like dust disks, are ubiquitous around young PMS stars in regions of isolated star formation, and that a large fraction of them have Rout>300AU. It also shows the potential of the CN N=2-1 transition to probe the kinematics of these disks, thereby measuring the stellar mass, using high resolution observations with ALMA.

Abstract Copyright:

Journal keyword(s): radio lines: planetary systems - stars: pre-main sequence - circumstellar matter - protoplanetary disks

Simbad objects: 54

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Number of rows : 54

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 V* FN Tau Or* 04 14 14.5943659839 +28 27 58.063377983     14.70 13.68   M5 141 0
2 V* CW Tau Or* 04 14 17.0041128798 +28 10 57.765657757 13.92 13.64 12.36 12.86   K0Ve 315 0
3 [BCG93] 1 TT* 04 14 17.6094853639 +28 06 09.650035718 18.04         M4.5 73 0
4 V* CY Tau Or* 04 17 33.7281514373 +28 20 46.809969664 14.52 14.68 13.40 12.59   M1.5 229 0
5 V* BP Tau Or* 04 19 15.8342975037 +29 06 26.929456808   13.13 12.12 11.89   K5/7Ve 599 0
6 V* DE Tau Or* 04 21 55.6346296353 +27 55 06.184221341 15.18 15.13 13.80     M3Ve 222 0
7 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 649 1
8 V* T Tau Or* 04 21 59.4323326335 +19 32 06.439974179   11.01 9.30 9.80   K0IV/Ve 1249 2
9 NAME T Tau N *i* 04 21 59.433 +19 32 06.42   11.22 10.12 9.80   K1.5 164 1
10 V* FS Tau Or* 04 22 02.1925017485 +26 57 30.331063489 17.57   14.10 15.63   M3.5e+M0e 257 0
11 V* FT Tau Or* 04 23 39.1894939930 +24 56 14.248383831   16.15 14.93 14.70   M2.8 109 0
12 2MASS J04270266+2605304 Y*O 04 27 02.66593 +26 05 30.3790           ~ 135 0
13 V* DG Tau Or* 04 27 04.6913654419 +26 06 16.041555299 13.57 13.97 10.50 12.28   K6Ve 923 1
14 V* GV Tau TT* 04 29 23.7314759229 +24 33 00.216016292 19.20         K7 271 2
15 V* IQ Tau Or* 04 29 51.5569553814 +26 06 44.854858369 15.43   13.80 12.28 11.11 M0.5 198 0
16 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1217 0
17 EM* LkHA 358 TT* 04 31 36.1396524070 +18 13 43.176961457     19.0     M0.9 87 0
18 V* V1213 Tau Or* 04 31 37.47192 +18 12 24.4800           K7 516 0
19 V* HL Tau Or* 04 31 38.471952 +18 13 58.08504   15.89 14.49 14.39   K5 1201 0
20 IRAS 04287+1807 mul 04 31 38.8 +18 13 57           ~ 796 0
21 V* HK Tau Or* 04 31 50.5722969258 +24 24 17.775488652 16.81   15.10     M0.5 295 1
22 NAME HK Tau B TT* 04 31 50.58 +24 24 16.4           M1 66 0
23 Haro 6-13 Or* 04 32 15.4177438039 +24 28 59.580866027 19.22   17.7     M0 181 1
24 V* GG Tau Or* 04 32 30.3318954228 +17 31 40.834888327 14.84 14.78 13.40 11.54   M0e+M2.0e 647 1
25 V* UZ Tau B TT* 04 32 42.82968 +25 52 31.4148   14.07 12.72 13.35   M1/3Ve 136 0
26 V* UZ Tau ** 04 32 43.02168 +25 52 30.9036           M4Ve+M1/3Ve 285 0
27 IRAS 04302+2247 Y*O 04 33 16.50096 +22 53 20.4000           ~ 135 0
28 V* DL Tau Or* 04 33 39.0766866461 +25 20 38.097973550 14.04 14.59 13.40 11.85 10.89 K7Ve 282 0
29 V* DM Tau Or* 04 33 48.7335659850 +18 10 09.974471722 14.30 14.82 14.00     M2Ve 510 0
30 V* CI Tau Or* 04 33 52.0144455735 +22 50 30.093741884 14.97 15.09 13.80     K4IVe 261 1
31 V* AA Tau Or* 04 34 55.4222683130 +24 28 53.038273587 13.14 13.34 12.20     K5Ve 626 0
32 V* DN Tau Or* 04 35 27.3776240781 +24 14 58.908761629 13.56 12.88 11.50 11.79   M1:Ve 348 0
33 V* DO Tau Or* 04 38 28.5882167490 +26 10 49.472067634 12.78 13.44 12.30 13.01   M1Ve 313 1
34 V* HV Tau C TT* 04 38 35.5121708248 +26 10 41.334466864         14.90 K6 87 0
35 EM* LkCa 15 Or* 04 39 17.7912813350 +22 21 03.387667491   13.01 12.03 11.61   K5:Ve 552 1
36 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3479 0
37 Haro 6-33 TT* 04 41 38.8300758211 +25 56 26.681998749     18.40     M0.5 100 2
38 V* GO Tau Or* 04 43 03.0761884276 +25 20 18.708294279   16.2 14.40     M2.3 151 0
39 V* DQ Tau Or* 04 46 53.0577037389 +17 00 00.135310040 14.56 13.67 12.00 13.21   M1Ve 286 0
40 V* DR Tau Or* 04 47 06.2152696011 +16 58 42.814250257 12.03 11.86 10.50 12.19   K5Ve 467 0
41 V* DS Tau Or* 04 47 48.5954846337 +29 25 11.189809829 13.11 13.16 12.30 12.37 10.80 K4Ve 208 0
42 V* UY Aur Or* 04 51 47.3900418279 +30 47 13.552212742 12.82 12.96 11.90 10.59 9.52 M0e+M2.5e 326 0
43 V* GM Aur Or* 04 55 10.9813656049 +30 21 59.375978047 14.59 14.22 13.10     K3Ve 552 0
44 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 932 2
45 V* SU Aur Or* 04 55 59.3861369488 +30 34 01.499800471   10.33 9.30 9.17   G2IIIne 534 0
46 HD 31648 Ae* 04 58 46.2654165113 +29 50 36.990341242 7.84 7.78 7.62 7.76 7.43 A5Vep 394 0
47 NAME CB 26 YSO 1 Y*O 04 59 50.793 +52 04 43.87           ~ 10 1
48 2MASS J05044139+2509544 TT* 05 04 41.3974730845 +25 09 54.581861436           M3.7 38 0
49 2MASS J05062332+2432199 TT* 05 06 23.3325973176 +24 32 19.923493583           M3/5e 37 0
50 V* RW Aur TT* 05 07 49.5662483 +30 24 05.177426   10.86 9.60 9.95   K1/5e+K5e 708 0
51 HD 36112 Ae* 05 30 27.5286772598 +25 19 57.082162439   8.57 8.27     A8Ve 358 0
52 V* CQ Tau Ae* 05 35 58.4671238887 +24 44 54.086375712 11.290 10.780 10.000   8.33 F5IVe 255 0
53 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3027 0
54 HD 163296 Ae* 17 56 21.2882188601 -21 57 21.872343282 7.00 6.93 6.85 6.86 6.67 A1Vep 803 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-01:02:30

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