2008A&A...489..601M


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.12CET00:41:46

2008A&A...489..601M - Astronomy and Astrophysics, volume 489, 601-605 (2008/10-2)

Searching for molecular hydrogen mid-infrared emission in the circumstellar environments of Herbig Be stars.

MARTIN-ZAIEDI C., VAN DISHOECK E.F., AUGEREAU J.-C., LAGAGE P.-O. and PANTIN E.

Abstract (from CDS):

Molecular hydrogen (H2) is the most abundant molecule in the circumstellar (CS) environments of young stars, and is a key element in giant planet formation. The measurement of the H2 content provides the most direct probe of the total amount of CS gas, especially in the inner warm planet-forming regions of the disks. Most Herbig Be stars (HBes) are distant from the Sun and their nature and evolution are still debated. We therefore conducted mid-infrared observations of H2 as a tracer of warm gas around HBes known to have gas-rich CS environments. We report a search for the H2 S(1) emission line at 17.0348µm in the CS environments of 5 HBes with the high resolution spectroscopic mode of VISIR (ESO VLT Imager and Spectrometer for the mid-InfraRed). No source shows evidence for H2 emission at 17.0348µm. Stringent 3σ upper limits on the integrated line fluxes are derived. Depending on the adopted temperature, limits on column densities and masses of warm gas are also estimated. These non-detections constrain the amount of warm (>150K) gas in the immediate CS environments of our target stars to be less than ∼1-10MJup.

Abstract Copyright:

Journal keyword(s): stars: circumstellar matter - stars: formation - stars: pre-main sequence - ISM: molecules

Simbad objects: 10

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Number of rows : 10

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 * gam Eri LP? 03 58 01.7669489 -13 30 30.669770 6.52 4.54 2.94 1.68 0.68 M0III-IIIb 168 0
2 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 899 2
3 * bet Col PM* 05 50 57.5921991 -35 46 05.915211 5.49 4.28 3.12 2.27 1.69 K1III_CN+1 132 0
4 HD 250550 Ae* 06 01 59.9894900068 +16 30 56.724889160   9.60 9.593 9.64   B9e 228 1
5 HD 45677 Be* 06 28 17.4219761127 -13 03 11.130589443 7.86 8.52 8.50 8.11 8.01 B2IV/V[e] 299 0
6 HD 259431 Ae* 06 33 05.1905483916 +10 19 19.987469692 8.39 8.95 8.72     B6ep 257 1
7 HD 76534 Be* 08 55 08.70673 -43 27 59.8852 7.04 7.62 7.50     B2Vn 110 2
8 * nu. Hya PM* 10 49 37.4887449 -16 11 37.135989 5.62 4.35 3.11 2.17 1.53 K1.5IIIHdel-0.5 154 0
9 HD 97048 Ae* 11 08 03.3105687971 -77 39 17.491180130 9.03 8.76 9.00   8.64 A0Vep 436 0
10 HD 98922 Be* 11 22 31.6740564115 -53 22 11.456030308   6.80 6.76     B9Ve 110 1

    Equat.    Gal    SGal    Ecl

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2019.11.12-00:41:46

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