High mass‐loss asymptotic giant branch stars detected by the midcourse space experiment in the ‘intermediate’ and ‘outer’ galactic bulge

Ojha, D. K. ; Tej, A. ; Schultheis, M. ; Omont, A. ; Schuller, F. (2007) High mass‐loss asymptotic giant branch stars detected by the midcourse space experiment in the ‘intermediate’ and ‘outer’ galactic bulge Monthly Notices of the Royal Astronomical Society, 381 (3). pp. 1219-1234. ISSN 0035-8711

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Official URL: https://academic.oup.com/mnras/article/381/3/1219/...

Related URL: http://dx.doi.org/10.1111/j.1365-2966.2007.12320.x

Abstract

We present a study of Midcourse Space Experiment (MSX) point sources in the Galactic bulge (|l| < 3°, 1° < |b| < 5°), observed in the A, C, D and E bands (8-21μm), with a total area ∼48 deg2 and more than 7000 detected sources in the MSX D band (15 μm). We discuss the nature of the MSX sources [mostly asymptotic giant branch (AGB) stars], their luminosities, the interstellar extinction, the mass‐loss rate distribution and the total mass‐loss rate in the bulge. The mid‐infrared data of MSX point sources have been combined with the near‐infrared (J, H and Ks) data of Two Micron All Sky Survey. The cross‐identification was restricted to Ks-band detected sources with Ks ≤ 11 mag. However, for those bright MSX D-band sources ([D] < 4.0 mag), which do not satisfy this criterion, we have set no Ks-band magnitude cut‐off. The bolometric magnitudes and the corresponding luminosities of the MSX sources were derived by fitting blackbody curves. The relation between M and (Ks-[15])0 was used to derive the mass‐loss rate of each MSX source in the bulge fields. Except for very few post‐AGB stars, planetary nebulae and OH/IR stars, a large fraction of the detected sources at 15 μm (MSX D band) are AGB stars well above the red giant branch tip. A number of them show an excess in ([A]−[D])0 and (Ks−[D])0 colours, characteristic of mass‐loss. These colours, especially (Ks−[D])0, enable estimation of the mass‐loss rates forumla of the sources in the bulge fields which range from 10−7 to 10−4 M yr−1. Taking into consideration the completeness of the mass‐loss rate bins, we find that the contribution to the integrated mass‐loss is probably dominated by mass‐loss rates larger than 3 × 10−7 M yr−1 and is about 1.96 × 10−4 M yr−1 deg−2 in the ‘intermediate’ and ‘outer’ bulge fields of sources with mass‐loss rates, M > 3×10−7 M yr−1. The corresponding integrated mass‐loss rate per unit stellar mass is 0.48 × 10−11 yr−1. Apart from this, the various mid- and near-infrared colour–colour and colour–magnitude diagrams are discussed in the paper to study the nature of the stellar population in the MSX bulge fields.

Item Type:Article
Source:Copyright of this article belongs to Royal Astronomical Society.
Keywords:Stars: AGB And Post‐AGB; Circumstellar Matter; Stars: Mass‐Loss; Dust; Extinction; Infrared: Stars
ID Code:104355
Deposited On:16 May 2017 11:05
Last Modified:16 May 2017 11:05

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