Astronomy:IRAS 07598+6508

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IRAS 07598+6508
IRAS 07598+6508 taken with Pan-STARRS
Observation data (J2000.0 epoch)
ConstellationCamelopardalis
Right ascension 08h 04m 30.46s
Declination+64° 59′ 52.87″
Redshift0.148839
Helio radial velocity44,621 km/s
Distance2.377 Mly (726.64 Mpc)
Apparent magnitude (V)15.5
Apparent magnitude (B)14.3
Characteristics
TypeBALQSO, Sy1
Notable featuresLuminous infrared galaxy, galaxy merger
Other designations
LEDA 97524, IRAS F07599+6508, BIG 222b, 2XMM J080430.4+645951

IRAS 07598+6508 known as IRAS F07599+6508, is a quasar located in the constellation of Camelopardalis. It is located 2.37 billion light years from Earth and is classified as both an ultraluminous infrared galaxy and a Seyfert galaxy.[1]

Characteristics

IRAS 07598+6508 is categorized an advanced galaxy merger. It shows several tidal features according to ground-based optical images.[2] A patchy emission is found having a low-surface brightness of around 22 R magnitude arcsec−2 ,based on Hubble Space Telescope (HST) imaging on the host galaxy. This emission is suggestive of tidal debris created by a recent galaxy-to-galaxy interaction.[3] A deep R-band image reveals the presence of an extended tidal tail from north to east direction. It has a dynamical age of ~ 160 Myr and is curving towards south of the nucleus by ~ 50 kiloparsecs (kpc). Since one tidal tail is clearly seen, the merger was probably caused from the interaction of a spiral and elliptical galaxy.[4]

In addition, IRAS 07598+6508 has several star clusters located both west and south, based on a HST optical image.[5] The galaxy is infrared bright with a source having an estimated luminosity of L2-10keV = 1.12 x 1042 erg s−1.[6]

IRAS 07598+6508 is a low-redshift broad absorption line quasar according to Sebastian Lipari[7] and by ROSAT.[8] It shows abnormally large blueshifts by 3000 km s−1 to a Balmer line as well as sodium (Na I) λ5892 at emission peaks. When looking at both Hα and Hβ intensity ratios, a broad emission line in IRAS 07598+6508 is found reddening by E(B-V) ~ 0.45 with a reddening of a spectral energy distribution of E(B-V) ~ 0.12.[9]

IRAS 07598+6508 is also known to be a strong ferrous (Fe II) emitter although X-ray quiet with a value of αox = 2.45.[10] It has a spectrum being influenced by its tapered broad line region with a full width at half maximum measurement of 1780 km s−1. Besides iron, IRAS 07598+6508 emits spectral lines of titanium (Ti II) and chromium (Cr II).[11] Given its strong Fe II emission, the emission likely derived from a superbubble or was caused by ejected material from a type II supernovae.[7]

Optical HST imaging found two emission clumps, located ~ 7" southeast and south from IRAS 07598+6508. This presence of clumps indicates the emission originates from OB associations and is the key to signs of recent star formation in the galaxy.[12] A NICMOS image of IRAS 07598+6508, finds electromagnetic radiation is controlled by a source of light from the nucleus although low-level emission is also visible right up to ~ 2" radius.[5]

References

  1. ↑ "Your NED Search Results". https://ned.ipac.caltech.edu/cgi-bin/objsearch?search_type=Obj_id&objid=61690&objname=1&img_stamp=YES&hconst=73.0&omegam=0.27&omegav=0.73&corr_z=1. 
  2. ↑ A. Surface, Jason; Sanders, D.B.; D. Vacca, William (January 1998). "HST/WFPC2 Observations of Warm Ultraluminous Infrared Galaxies". The Astrophysical Journal 492 (1): 116–136. doi:10.1086/305028. Bibcode: 1998ApJ...492..116S. https://iopscience.iop.org/article/10.1086/305028/fulltext/. 
  3. ↑ Joyce, P.J.; Disney, M.J.; Blades, J.C.; Boksenberg, A.; Crane, P. (December 1996). "The Host Galaxies of IRAS-Selected Quasi-Stellar Objects". The Astrophysical Journal 473 (2): 760–762. doi:10.1086/178187. Bibcode: 1996ApJ...473..760B. https://iopscience.iop.org/article/10.1086/178187/pdf. 
  4. ↑ Canalizo, Gabriela; Stockton, Alan (October 2000). "Stellar Populations in the Host Galaxies of Markarian 1014, IRAS 07598+6508, and Markarian 231". The Astronomical Journal 120 (4): 1750–1763. doi:10.1086/301585. ISSN 0004-6256. Bibcode: 2000AJ....120.1750C. http://dx.doi.org/10.1086/301585. 
  5. ↑ 5.0 5.1 Scoville, N.Z.; Evans, A.S.; Thompson, R.; Rieke, M.; Hines, D.C.; Low, F.J.; Dinshaw, N.; Surface, J.A. et al. (March 2000). "NICMOS Imaging of Infrared-Luminous Galaxies". The Astronomical Journal 119 (3): 991–1061. doi:10.1086/301248. Bibcode: 2000AJ....119..991S. https://iopscience.iop.org/article/10.1086/301248/fulltext/. 
  6. ↑ Laha, Sibasish; Guainazzi, Matteo; Piconcelli, Enrico; Gandhi, Poshak; Ricci, Claudio; Ghosh, Ritesh; Markowitz, Alex G.; Bagchi, Joydeep (2018-11-13). "A Study of X-Ray Emission of Galaxies Hosting Molecular Outflows (MOX Sample)". The Astrophysical Journal 868 (1): 10. doi:10.3847/1538-4357/aae390. ISSN 0004-637X. Bibcode: 2018ApJ...868...10L. 
  7. ↑ 7.0 7.1 Lipari, Sebastian (November 1994). "Galaxies with extreme infrared and Fe II emission. 2: IRAS 07598+6508: A starburst/young broad absorption line QSO". The Astrophysical Journal 436: 102. doi:10.1086/174884. ISSN 0004-637X. Bibcode: 1994ApJ...436..102L. http://dx.doi.org/10.1086/174884. 
  8. ↑ Gallagher, S.C.; Brandt, W.N.; Sambruna, R.M. (July 1999). "Exploratory ASCA Observations of Broad Absorption Line Quasi-stellar Objects". The Astrophysical Journal 519 (2): 549–555. doi:10.1086/307405. Bibcode: 1999ApJ...519..549G. https://iopscience.iop.org/article/10.1086/307405/fulltext/. 
  9. ↑ Hines, Dean C.; Wills, Beverley J. (1995-08-01). "The Polarized Spectrum of the Fe [CSCii[/CSC]–Rich Broad Absorption Line QSO IRAS 07598+6508"]. The Astrophysical Journal 448 (2). doi:10.1086/309611. ISSN 0004-637X. http://dx.doi.org/10.1086/309611. 
  10. ↑ Lawrence, A.; Elvis, M.; Wilkes, B. J.; McHardy, I.; Brandt, N. (1997-03-11). "X-ray and optical continua of active galactic nuclei with extreme Fe II emission". Monthly Notices of the Royal Astronomical Society 285 (4): 879–890. doi:10.1093/mnras/285.4.879. ISSN 0035-8711. 
  11. ↑ Veron, M.-P.; Joly, M.; Veron, P.; Boroson, T.; Lipari, S.; Ogle, P. (June 2006). "The emission spectrum of the strong Fe II emitter BAL Seyfert 1 galaxy IRAS 07598+6508". Astronomy & Astrophysics 451 (3): 851–858. doi:10.1051/0004-6361:20054237. ISSN 0004-6361. Bibcode: 2006A&A...451..851V. 
  12. ↑ Tacconi, L.J.; Genzel, R.; Lutz, D.; Rigopoulou, D.; Baker, A.J.; Baker, A.J.; Iserlohe, C.; Tecza, M. (November 2002). Ultraluminous IR Galaxies: QSOs in Formation?. doi:10.1086/343075. https://iopscience.iop.org/article/10.1086/343075/fulltext/56010.text.html#tb4. Retrieved 2024-10-06. 



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