2013A&A...559A..84M


Query : 2013A&A...559A..84M

2013A&A...559A..84M - Astronomy and Astrophysics, volume 559A, 84-84 (2013/11-1)

DIGIT survey of far-infrared lines from protoplanetary discs. II. CO.

MEEUS G., SALYK C., BRUDERER S., FEDELE D., MAASKANT K., EVANS II N.J., VAN DISHOECK E.F., MONTESINOS B., HERCZEG G., BOUWMAN J., GREEN J.D., DOMINIK C., HENNING T., VICENTE S. (The DIGIT Team)

Abstract (from CDS):

CO is an important component of a protoplanetary disc as it is one of the most abundant gas phase species. Furthermore, observations of CO transitions can be used as a diagnostic of the gas, tracing conditions in both the inner and outer disc. We present Herschel/PACS spectroscopy of a sample of 22 Herbig Ae/Be (HAEBEs) and eight T Tauri stars (TTS), covering the pure rotational CO transitions from J=14-> 13 up to J=49->48. CO is detected in only five HAEBEs, namely AB Aur, HD36112, HD97048, HD100546, and IRS 48, and in four TTS, namely AS 205, S CrA, RU Lup, and DG Tau. The highest transition detected is J=36->35 with Eup of 3669K, seen in HD100546 and DG Tau. We construct rotational diagrams for the discs with at least three CO detections to derive Trot and find average temperatures of 270K for the HAEBEs and 485K for the TTS. The HD100546 star requires an extra temperature component at Trot∼900-1000K, suggesting a range of temperatures in its disc atmosphere, which is consistent with thermo-chemical disc models. In HAEBEs, the objects with CO detections all have flared discs in which the gas and dust are thermally decoupled. We use a small model grid to analyse our observations and find that an increased amount of flaring means higher line flux, as it increases the mass in warm gas. CO is not detected in our flat discs as the emission is below the detection limit. We find that HAEBE sources with CO detections have high LUV and strong PAH emission, which is again connected to the heating of the gas. In TTS, the objects with CO detections are all sources with evidence of a disc wind or outflow. For both groups of objects, sources with CO detections generally have high UV luminosity (either stellar in HAEBEs or due to accretion in TTS), but this is not a sufficient condition for the detection of the far-IR CO lines.

Abstract Copyright:

Journal keyword(s): circumstellar matter - protoplanetary disks

Simbad objects: 31

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Number of rows : 31
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 V* DG Tau Or* 04 27 04.6921275888 +26 06 16.060169268 13.57 13.97 10.50 12.28   K6Ve 1000 1
2 V* AB Aur Ae* 04 55 45.8458932216 +30 33 04.292077032 7.20 7.16 7.05 6.96 6.70 A0Ve 1012 2
3 HD 35187 Y*O 05 24 01.17261 +24 57 37.5791   8.79 8.71 8.72   A2e+A7 102 0
4 HD 36112 Ae* 05 30 27.5285630040 +25 19 57.076288752   8.57 8.27     A8Ve 428 0
5 HD 38120 Be* 05 43 11.8932782280 -04 59 49.889995692 9.08 9.10 9.1     B9Vnne 83 0
6 HD 50138 Ae* 06 51 33.3989823840 -06 57 59.450772852 6.28 6.68 6.67     A1Ib/II 214 0
7 HD 97048 Ae* 11 08 03.3109731720 -77 39 17.490777444 9.03 8.76 9.00   8.64 A0Vep 515 0
8 HD 98922 Be* 11 22 31.6743077592 -53 22 11.457008148   6.80 6.76     B9Ve 126 1
9 HD 100453 Ae* 11 33 05.5766482920 -54 19 28.547100696   8.09 7.79     A9Ve 253 1
10 HD 100546 Be* 11 33 25.4408872296 -70 11 41.241297948   6.71 6.30   6.64 A0VaekB8_lB 744 1
11 V* DX Cha Ae* 12 00 05.0868602544 -78 11 34.565724312   6.81 6.60     A0_sh 330 0
12 CPD-36 6759 Y*O 15 15 48.4460065200 -37 09 16.024369824   9.21 8.708     F8V 424 1
13 HD 135344 * 15 15 48.9462675744 -37 08 55.731368400   7.84 7.76     A0V 140 1
14 HD 139614 Ae? 15 40 46.3820275416 -42 29 53.538761832   8.47 8.24     A9VekA5mA5(_lB) 193 0
15 CD-33 10685 Or* 15 45 12.8678037432 -34 17 30.644403036 12.47 11.56 10.224 9.60 8.685 K3Ve 253 1
16 HD 141569 Y*O 15 49 57.7482550392 -03 55 16.341617064 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 510 0
17 HD 142666 TT* 15 56 40.0221861696 -22 01 40.005872148 9.41 9.37 8.82 8.31 8.01 F0V_sh 246 0
18 HD 142527 Ae* 15 56 41.8882637904 -42 19 23.248281828   9.04 8.34     F6III 582 1
19 V* RU Lup TT* 15 56 42.3108692112 -37 49 15.473946900 9.27 10.07 9.60     K7/M0e 432 0
20 V* RY Lup Or* 15 59 28.3864710696 -40 21 51.249496176   12.62 9.90     G8/K1IV-V 204 0
21 HD 144432 Ae* 16 06 57.9533126832 -27 43 09.760564056 8.47 8.53 8.19 7.82 7.53 A9/F0V 230 1
22 V* V856 Sco Ae* 16 08 34.2870044544 -39 06 18.325711332 7.66 7.41 7.05 6.92   A7IIIne_sh 374 0
23 V* V866 Sco Or* 16 11 31.345632 -18 38 25.96200   13.98 12.63 12.81   K0e+K5e 269 0
24 EM* SR 21A TT* 16 27 10.2778380120 -24 19 12.622467720   16.08 14.10     G1 262 1
25 IRAS 16245-2423 TT* 16 27 37.1906433768 -24 30 35.025246828       16.66 14.67 B5-F2 274 0
26 V* V1003 Oph TT* 16 34 09.1696133088 -15 48 16.776092124     13.44     G5 94 0
27 HD 150193 Be* 16 40 17.9243127240 -23 53 45.193372692 9.69 9.32 8.79 8.41   B9.5Ve 307 0
28 HD 163296 Ae* 17 56 21.2881851168 -21 57 21.871819008 7.00 6.93 6.85 6.86 6.67 A1Vep 1002 0
29 HD 169142 Ae* 18 24 29.7799891464 -29 46 49.327400568   8.42 8.16     F1VekA3mA3_lB? 408 2
30 V* S CrA Or* 19 01 08.597088 -36 57 19.89504   11.76 10.91 11.41   G0Ve+K0Ve 271 0
31 HD 179218 Ae* 19 11 11.2538919456 +15 47 15.636008472 7.55 7.476 7.39 7.25 7.21 A0Ve 241 0

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2023.01.30-23:25:13

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