IRAS 15099-5856: REMARKABLE MID-INFRARED SOURCE WITH PROMINENT CRYSTALLINE SILICATE EMISSION EMBEDDED IN THE SUPERNOVA REMNANT MSH15-52

Journal Article · Sun May 01 00:00:00 EDT 2011 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/732/1/6· OSTI ID:21574677

Koo, Bon-Chul; Kim, Hyun-Jeong; Im, Myungshin ^[1]; McKee, Christopher F ^[2]; Suh, Kyung-Won ^[3]; Moon, Dae-Sik; Lee, Ho-Gyu ^[4]; Onaka, Takashi ^[5]; Burton, Michael G ^[6]; Hiramatsu, Masaaki ^[7]; Bessell, Michael S ^[8]; Gaensler, B M ^[9]; Lee, Jae-Joon ^[10]; Jeong, Woong-Seob ^[11]; Tatematsu, Ken'ichi; Kawabe, Ryohei; Ezawa, Hajime ^[12]; Kohno, Kotaro ^[13]; Wilson, Grant

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1. Department of Physics and Astronomy, Seoul National University, Seoul 151-742 (Korea, Republic of)
2. Department of Physics and Astronomy, University of California, Berkeley, CA 94720 (United States)
3. Department of Astronomy and Space Science, Chungbuk National University, Cheingju-City 361-763 (Korea, Republic of)
4. Department of Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H4 (Canada)
5. Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113-0033 (Japan)
6. School of Physics, University of New South Wales, Sydney, New South Wales 2052 (Australia)
7. Academia Sinica Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 10617, Taiwan (China)
8. Research School of Astronomy and Astrophysics, Mount Stromlo Observatory (Australia)
9. Sydney Institute for Astronomy, School of Physics, The University of Sydney, NSW 2006 (Australia)
10. Astronomy and Astrophysics Department, Pennsylvania State University, University Park, PA 16802 (United States)
11. Korea Astronomy and Space Science Institute, 61-1, Whaam-dong, Yuseong-gu, Daejeon 305-348 (Korea, Republic of)
12. National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo 181-8588 (Japan)
13. Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015 (Japan)

We report new mid-infrared (MIR) observations of the remarkable object IRAS 15099-5856 using the space telescopes AKARI and Spitzer, which demonstrate the presence of prominent crystalline silicate emission in this bright source. IRAS 15099-5856 has a complex morphology with a bright central compact source (IRS1) surrounded by knots, spurs, and several extended ({approx}4') arc-like filaments. The source is seen only at {>=}10 {mu}m. The Spitzer mid-infrared spectrum of IRS1 shows prominent emission features from Mg-rich crystalline silicates, strong [Ne II] 12.81 {mu}m, and several other faint ionic lines. We model the MIR spectrum as thermal emission from dust and compare with the Herbig Be star HD 100546 and the luminous blue variable R71, which show very similar MIR spectra. Molecular line observations reveal two molecular clouds around the source, but no associated dense molecular cores. We suggest that IRS1 is heated by UV radiation from the adjacent O star Muzzio 10 and that its crystalline silicates most likely originated in a mass outflow from the progenitor of the supernova remnant (SNR) MSH 15-52. IRS1, which is embedded in the SNR, could have been shielded from the SN blast wave if the progenitor was in a close binary system with Muzzio 10. If MSH 15-52 is a remnant of Type Ib/c supernova (SN Ib/c), as has been previously proposed, this would confirm the binary model for SN Ib/c. IRS1 and the associated structures may be the relics of massive star death, as shaped by the supernova explosion, the pulsar wind, and the intense ionizing radiation of the embedded O star.

• OSTI ID: 21574677
• Journal Information: Astrophysical Journal, Vol. 732, Issue 1; Other Information: DOI: 10.1088/0004-637X/732/1/6; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
DUSTS
EMISSION
INFRARED SPECTRA
SILICATES
SUPERNOVA REMNANTS
COSMIC RADIO SOURCES
OXYGEN COMPOUNDS
SILICON COMPOUNDS
SPECTRA