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


Query : 2013A&A...549A..92G

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: 53

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Number of rows : 53
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 V* FN Tau Or* 04 14 14.5945463760 +28 27 58.067731188     14.70 13.68   M5 150 0
2 V* CW Tau Or* 04 14 17.0042670144 +28 10 57.766508508 13.92 13.64 12.36 12.86   K0Ve 334 0
3 [BCG93] 1 TT* 04 14 17.6095515480 +28 06 09.654704388 18.04         M4.5 85 0
4 V* CY Tau Or* 04 17 33.7284990744 +28 20 46.812121656 14.52 14.68 13.40 12.59   M1.5 250 0
5 V* BP Tau Or* 04 19 15.8339827632 +29 06 26.926959492   13.13 12.12 11.89   K5/7Ve 632 0
6 V* DE Tau Or* 04 21 55.6347850824 +27 55 06.184016436 15.18 15.13 13.80     M3Ve 238 0
7 V* RY Tau Or* 04 21 57.4092550080 +28 26 35.555316612 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 673 1
8 V* T Tau TT* 04 21 59.4319873992 +19 32 06.432393336   11.22 10.12 9.80   K0IV/Ve 1364 1
9 V* FS Tau Or* 04 22 02.1798627024 +26 57 30.575293308 17.57   14.10 15.63   M3.5e+M0e 267 0
10 V* FT Tau Or* 04 23 39.1888788312 +24 56 14.250818940   16.15 14.93 14.70   M2.8 126 0
11 [EM98] DG Tau B cRN Y*O 04 27 02.66088 +26 05 30.4548           ~ 157 0
12 V* DG Tau Or* 04 27 04.6921275888 +26 06 16.060169268 13.57 13.97 10.50 12.28   K6Ve 981 1
13 V* GV Tau TT* 04 29 23.7314759229 +24 33 00.216016292 19.20         K7 278 0
14 V* IQ Tau Or* 04 29 51.5569574040 +26 06 44.859710736 15.43   13.80 12.28 11.11 M0.5 217 0
15 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1294 0
16 EM* LkHA 358 TT* 04 31 36.1433863008 +18 13 43.204853460     19.0     M0.9 89 0
17 V* V1213 Tau Or* 04 31 37.5055489536 +18 12 24.383952396           K7 540 0
18 V* HL Tau Or* 04 31 38.5107609312 +18 13 57.859747968   15.89 14.49 14.39   K5 1319 0
19 IRAS 04287+1807 mul 04 31 38.8 +18 13 57           ~ 796 0
20 V* HK Tau TT* 04 31 50.5715875272 +24 24 17.775307548 16.81 16.689 15.292     M0.5 319 1
21 V* HK Tau B TT* 04 31 50.6002481212 +24 24 15.502558869           ~ 74 0
22 Haro 6-13 Or* 04 32 15.4174258632 +24 28 59.577717108 19.22   17.7     M0 195 1
23 V* GG Tau Or* 04 32 30.3506925552 +17 31 40.494063144 14.84 14.78 13.40 11.54   M0e+M2.0e 692 1
24 V* UZ Tau Y*O 04 32 42.81 +25 52 31.3           M4Ve+M1/3Ve 297 0
25 V* UZ Tau B TT* 04 32 42.8118779016 +25 52 31.198173600   14.07 12.72 13.35   M1/3Ve 142 0
26 IRAS 04302+2247 Y*O 04 33 16.50096 +22 53 20.4000           ~ 155 0
27 V* DL Tau Or* 04 33 39.0767679288 +25 20 38.101382952 14.04 14.59 13.40 11.85 10.89 K7Ve 308 0
28 V* DM Tau Or* 04 33 48.7336763736 +18 10 09.973460280 14.30 14.82 14.00     M2Ve 579 0
29 V* CI Tau Or* 04 33 52.0143963264 +22 50 30.094090908 14.97 15.09 13.80     K4IVe 307 1
30 V* AA Tau Or* 04 34 55.4201902392 +24 28 53.033624580 13.14 13.34 12.20     K5Ve 679 0
31 V* DN Tau Or* 04 35 27.3776226144 +24 14 58.910343720 13.56 12.88 11.50 11.79   M1:Ve 367 0
32 V* DO Tau Or* 04 38 28.5880527336 +26 10 49.467596196 12.78 13.44 12.30 13.01   M1Ve 335 1
33 V* HV Tau C TT* 04 38 35.5125950280 +26 10 41.316576204         14.90 K6 91 0
34 EM* LkCa 15 Or* 04 39 17.7911622816 +22 21 03.390090984   13.01 12.03 11.61   K5:Ve 612 1
35 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3926 0
36 Haro 6-33 TT* 04 41 38.8257958224 +25 56 26.741499648     18.40     M0.5 111 2
37 V* GO Tau Or* 04 43 03.0761840904 +25 20 18.706850340   16.2 14.40     M2.3 174 0
38 V* DQ Tau Or* 04 46 53.0575226016 +17 00 00.136127304 14.56 13.67 12.00 13.21   M1Ve 311 0
39 V* DR Tau Or* 04 47 06.2151561264 +16 58 42.813872580 12.03 11.86 10.50 12.19   K5Ve 499 0
40 V* DS Tau Or* 04 47 48.5954691000 +29 25 11.191621512 13.11 13.16 12.30 12.37 10.80 K4Ve 230 0
41 V* UY Aur Or* 04 51 47.3890167432 +30 47 13.551561492 12.82 12.96 11.90 10.59 9.52 M0e+M2.5e 341 0
42 V* GM Aur Or* 04 55 10.9815576936 +30 21 59.373771876 14.59 13.351 12.242 11.798   K3Ve 616 0
43 V* AB Aur Ae* 04 55 45.8458932216 +30 33 04.292077032 7.20 7.16 7.05 6.96 6.70 A0Ve 992 2
44 V* SU Aur Or* 04 55 59.3866872552 +30 34 01.499608092   10.33 9.30 9.17   G2IIIne 562 0
45 HD 31648 Ae* 04 58 46.2655706952 +29 50 36.987625680 7.84 7.78 7.62 7.76 7.43 A5Vep 458 0
46 NAME CB 26 YSO 1 Y*O 04 59 50.793 +52 04 43.87           ~ 10 1
47 2MASS J05044139+2509544 TT* 05 04 41.3972186256 +25 09 54.583156908           M3.7 41 0
48 2MASS J05062332+2432199 TT* 05 06 23.3356482336 +24 32 19.917141360           M3/5e 38 0
49 V* RW Aur TT* 05 07 49.5662483 +30 24 05.177426   10.86 9.60 9.95   K1/5e+K5e 746 0
50 HD 36112 Ae* 05 30 27.5285630040 +25 19 57.076288752   8.57 8.27     A8Ve 416 0
51 V* CQ Tau Ae* 05 35 58.4666264136 +24 44 54.091450572 11.290 10.780 10.000   8.33 F5IVe 283 0
52 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3338 1
53 HD 163296 Ae* 17 56 21.2881851168 -21 57 21.871819008 7.00 6.93 6.85 6.86 6.67 A1Vep 953 0

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2022.05.28-23:02:18

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