2014A&A...565A..68R


Query : 2014A&A...565A..68R

2014A&A...565A..68R - Astronomy and Astrophysics, volume 565A, 68-68 (2014/5-1)

Gas and dust in the beta Pictoris moving group as seen by the Herschel Space Observatory.

RIVIERE-MARICHALAR P., BARRADO D., MONTESINOS B., DUCHENE G., BOUY H., PINTE C., MENARD F., DONALDSON J., EIROA C., KRIVOV A.V., KAMP I., MENDIGUTIA I., DENT W.R.F. and LILLO-BOX J.

Abstract (from CDS):

Debris discs are thought to be formed through the collisional grinding of planetesimals, and then can be considered as the outcome of planet formation. Understanding the properties of gas and dust in debris discs can help us comprehend the architecture of extrasolar planetary systems. Herschel Space Observatory far-infrared (IR) photometry and spectroscopy have provided a valuable dataset for the study of debris discs gas and dust composition. This paper is part of a series of papers devoted to the study of Herschel-PACS observations of young stellar associations. This work aims at studying the properties of discs in the beta Pictoris moving group (BPMG) through far-IR PACS observations of dust and gas. We obtained Herschel-PACS far-IR photometric observations at 70, 100, and 160µm of 19 BPMG members, together with spectroscopic observations for four of them. These observations were centred at 63.18µm and 157µm, aiming to detect [OI] and [CII] emission. We incorporated the new far-IR observations in the SED of BPMG members and fitted modified blackbody models to better characterise the dust content. We have detected far-IR excess emission towards nine BPMG members, including the first detection of an IR excess towards HD 29391.The star HD 172555, shows [OI] emission, while HD 181296 shows [CII] emission, expanding the short list of debris discs with a gas detection. No debris disc in BPMG is detected in both [OI] and [CII]. The discs show dust temperatures in the range 55-264K, with low dust masses (<6.6x10–5M to 0.2M) and radii from blackbody models in the range 3 to ∼82AU. All the objects with a gas detection are early spectral type stars with a hot dust component.

Abstract Copyright:

Journal keyword(s): astrobiology - circumstellar matter - stars: evolution - Kuiper belt: general - astrochemistry

Simbad objects: 33

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Number of rows : 33
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 NAME THA As* 00 00 -62.0           ~ 416 0
2 HD 203 PM* 00 06 50.0863238088 -23 06 27.145662264   6.547 6.173   5.74 F3V 120 0
3 * bet03 Tuc ** 00 32 43.9053745704 -63 01 53.402028960 5.15 5.13 5.09     A0V 119 0
4 * 49 Cet PM* 01 34 37.7786780856 -15 40 34.898673000   5.667 5.607   5.54 A1V 272 0
5 HD 14082B BY* 02 17 24.7369490496 +28 44 30.411007188   8.33 7.74     G2V 101 0
6 HD 14082 BY* 02 17 25.2869702592 +28 44 42.145069812   7.545 7.031 8.04   F5V 115 0
7 BD+30 397 PM* 02 27 29.2543096632 +30 58 24.596323968   11.3 10.12 9.32 8.78 K7V 95 1
8 BD+05 378 PM* 02 41 25.8882694248 +05 59 18.396173868   11.58 10.271   8.807 K6Ve 102 1
9 HD 21997 PM* 03 31 53.6470102728 -25 36 50.940001116   6.501 6.372   6.25 A3IV/V 142 0
10 * 51 Eri PM* 04 37 36.1326090888 -02 28 24.775726260   5.486 5.209     F0IV 207 0
11 StKM 1-497 TT* 04 37 37.4553491592 -02 29 28.950973764   12.04 10.59   8.59 M1.1V 119 0
12 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3975 0
13 HD 32297 * 05 02 27.4358754192 +07 27 39.678553260   8.32 8.14     A0V 173 0
14 V* AF Lep RS* 05 27 04.7633281608 -11 54 03.466002240   6.832 6.295     F8V(n)k: 221 0
15 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1789 1
16 V* AO Men PM* 06 18 28.2078302088 -72 02 41.447954904   11.06 9.809 9.299 8.456 K4Ve 129 0
17 HD 98800B SB* 11 22 05.288454 -24 46 39.04974   11.18 9.92     ~ 121 1
18 * alf Boo RG* 14 15 39.67207 +19 10 56.6730 2.46 1.18 -0.05 -1.03 -1.68 K1.5IIIFe-0.5 2232 0
19 HD 129391 * 14 41 51.5531398608 +18 29 45.162571416   8.55 7.51     G7III 16 0
20 HD 139084 Ro* 15 38 57.5566916952 -57 42 27.346084668   8.78 7.977   7.106 K0V 153 0
21 HD 141569 Y*O 15 49 57.7482550392 -03 55 16.341617064 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 501 0
22 * d Sco PM* 16 18 17.9001656 -28 36 50.476788   4.804 4.782     A1Va 154 0
23 * sig Her ** 16 34 06.1824264648 +42 26 13.234150680   4.177 4.196 6.02   B9V 189 0
24 * c Oph Be* 17 31 24.9541340 -23 57 45.513592 4.75 4.81 4.81 4.74 4.72 A0V 264 0
25 HD 164249 PM* 18 03 03.4097283792 -51 38 56.432149872   7.438 7.007 7.90   F6V 106 0
26 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2601 0
27 HD 172555 PM* 18 45 26.9009806435 -64 52 16.534807985   4.967 4.767     A7V 257 0
28 CD-64 1208 ** 18 45 37.0492713148 -64 51 45.888646069   10.518 9.433 9.694   K5Ve 60 0
29 V* PZ Tel BY* 18 53 05.8735056984 -50 10 49.897437168   9.22 8.342   7.464 G9IV 307 0
30 * eta Tel PM* 19 22 51.2060774616 -54 25 26.145617376   5.035 5.020   4.99 A0V 202 0
31 HD 181327 PM* 19 22 58.9437222504 -54 32 16.975668624   7.50 7.04   6.49 F6V 256 0
32 V* AT Mic Er* 20 41 51.15925 -32 26 06.8283 12.753 11.909 10.343 9.098 7.383 M4.5Ve+M4.5Ve 345 0
33 HD 199143 PM* 20 55 47.6748292416 -17 06 51.061731768   7.84 7.32 8.29   F8V 115 0

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2022.08.15-14:10:51

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