2014MNRAS.444.3911V


Query : 2014MNRAS.444.3911V

2014MNRAS.444.3911V - Mon. Not. R. Astron. Soc., 444, 3911-3925 (2014/November-2)

Signatures of warm carbon monoxide in protoplanetary discs observed with Herschel SPIRE.

VAN DER WIEL M.H.D., NAYLOR D.A., KAMP I., MENARD F., THI W.-F., WOITKE P., OLOFSSON G., PONTOPPIDAN K.M., DI FRANCESCO J., GLAUSER A.M., GREAVES J.S. and IVISON R.J.

Abstract (from CDS):

Molecular gas constitutes the dominant mass component of protoplanetary discs. To date, these sources have not been studied comprehensively at the longest far-infrared and shortest submillimetre wavelengths. This paper presents Herschel SPIRE FTS spectroscopic observations towards 18 protoplanetary discs, covering the entire 450-1540GHz (666-195 µm) range at ν/Δν ~ 400-1300. The spectra reveal clear detections of the dust continuum and, in six targets, a significant amount of spectral line emission primarily attributable to 12CO rotational lines. Other targets exhibit little to no detectable spectral lines. Low signal-to-noise detections also include signatures from 13CO, [Ci] and HCN. For completeness, we present upper limits of non-detected lines in all targets, including low-energy transitions of H2O and CH+ molecules. The 10 12CO lines that fall within the SPIRE FTS bands trace energy levels of ∼ 50-500K. Combined with lower and higher energy lines from the literature, we compare the CO rotational line energy distribution with detailed physical-chemical models, for sources where these are available and published. Our 13CO line detections in the disc around Herbig Be star HD 100546 exceed, by factors of ∼ 10–30, the values predicted by a model that matches a wealth of other observational constraints, including the SPIRE 12CO ladder. To explain the observed 12CO/13CO ratio, it may be necessary to consider the combined effects of optical depth and isotope selective (photo)chemical processes. Considering the full sample of 18 objects, we find that the strongest line emission is observed in discs around Herbig Ae/Be stars, although not all show line emission. In addition, two of the six T Tauri objects exhibit detectable 12CO lines in the SPIRE range.

Abstract Copyright: © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2014)

Journal keyword(s): astrochemistry - protoplanetary discs - circumstellar matter - stars: variables: T Tauri, Herbig Ae/Be

Simbad objects: 19

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Number of rows : 19
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* RY Tau Or* 04 21 57.4092550080 +28 26 35.555316612 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 677 1
2 V* FZ Tau Or* 04 32 31.7627107344 +24 20 03.056011548 16.15     15.04   M0 133 0
3 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4020 0
4 V* DR Tau Or* 04 47 06.2151561264 +16 58 42.813872580 12.03 11.86 10.50 12.19   K5Ve 503 0
5 V* AB Aur Ae* 04 55 45.8458932216 +30 33 04.292077032 7.20 7.16 7.05 6.96 6.70 A0Ve 1001 2
6 HD 36112 Ae* 05 30 27.5285630040 +25 19 57.076288752   8.57 8.27     A8Ve 421 0
7 HD 50138 Ae* 06 51 33.3989823840 -06 57 59.450772852 6.28 6.68 6.67     A1Ib/II 212 0
8 V* TW Hya TT* 11 01 51.9053285064 -34 42 17.033218380   11.94 10.50 10.626 9.18 K6Ve 1764 1
9 V* VW Cha Or* 11 08 01.3974165580 -77 42 28.579297348 13.91 14.04 12.80   10.69 K7+M0 174 0
10 HD 97048 Ae* 11 08 03.3109731720 -77 39 17.490777444 9.03 8.76 9.00   8.64 A0Vep 506 0
11 HD 100453 Ae* 11 33 05.5766482920 -54 19 28.547100696   8.09 7.79     A9Ve 248 1
12 HD 100546 Be* 11 33 25.4408872296 -70 11 41.241297948   6.71 6.30   6.64 A0VaekB8_lB 732 1
13 V* DX Cha Ae* 12 00 05.0868602544 -78 11 34.565724312   6.81 6.60     A0_sh 324 0
14 HD 142527 Ae* 15 56 41.8882637904 -42 19 23.248281828   9.04 8.34     F6III 572 1
15 HD 144432 Ae* 16 06 57.9533126832 -27 43 09.760564056 8.47 8.53 8.19 7.82 7.53 A9/F0V 229 1
16 V* V1003 Oph Or* 16 34 09.1696133088 -15 48 16.776092124     13.44     G5 94 0
17 HD 163296 Ae* 17 56 21.2881851168 -21 57 21.871819008 7.00 6.93 6.85 6.86 6.67 A1Vep 981 0
18 HD 169142 Ae* 18 24 29.7799891464 -29 46 49.327400568   8.42 8.16     F1VekA3mA3_lB? 400 2
19 HD 179218 Ae* 19 11 11.2538919456 +15 47 15.636008472 7.55 7.476 7.39 7.25 7.21 A0Ve 239 0

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2022.10.07-04:10:42

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