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IRAS 07598+6508

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IRAS 07598+6508
IRAS 07598+6508 taken with Pan-STARRS
Observation data (J2000.0 epoch)
ConstellationCamelopardalis
Right ascension08h 04m 30.46s
Declination+64° 59′ 52.87″
Redshift0.148839
Heliocentric 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

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IRAS 07598+6508 is categorized an advanced galaxy merger. It shows several tidal features according to ground-based optical images,[2] with a patchy emission found to have a low-surface brightness of around 22 R magnitude arcsec-2 resembling similarities to tidal debris created by a recent galaxy-to-galaxy interaction 40 kpc/500 km s-1 ~ 108 yr earlier.[3] There is a presence of an extended tidal tail from north to east direction, which it is seen arching south of the nucleus of around ~ 50 kiloparsecs (kpc). With a velocity of 300 km s-1 it has an estimated age of ~ 160 Myr. Since only one tail is found so far, the merger must have been caused through the interaction of a spiral and elliptical galaxy.[4]

In additional, IRAS 07598+6508 has several star clusters located both west and south.[5] The galaxy is infrared bright with a source estimated to have a luminosity of L2-10keV = 1.12 x 1042 erg s-1 and such contains wide emission lines.[6] It is also 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 iodide (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. Beside ferrous, IRAS 07598+6508 emits titanium oxide (Ti II) and chromium oxide (Cr II).[11] Given its strong Fe II emission, the emission likely derived from a superbubble or caused by ejected material from type II supernovae.[7]

Two emission clumps are located ~ 7" southeast and south from IRAS 07598+6508. This indicates the clumps are caused by emission originating from OB associations and is the key to a sign of recent star formation in the galaxy. Furthermore, a point-like nuclear emission is detected in three infrared bands although faint emission is seen. This indicates the nuclear emission might be well connected to star formation.[12]

References

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  1. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-10-06.
  2. ^ A. Surface, Jason; Sanders, D.B.; D. Vacca, William (January 1998). "HST/WFPC2 Observations of Warm Ultraluminous Infrared Galaxies". The Astrophysical Journal. 492: 116–136.
  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). doi:10.1086/178187.
  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.
  5. ^ Scoville, N.Z.; Evans, A.S.; Thompson, R.; Rieke, M.; Hines, D.C.; Low, F.J.; Dinshaw, N.; Surface, J.A.; Armus, L. (March 2000). "NICMOS Imaging of Infrared-Luminous Galaxies". The Astronomical Journal. 119.
  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.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  7. ^ a b 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.
  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: 549–555.
  9. ^ Hines, Dean C.; Wills, Beverley J. (1995-08-01). "The Polarized Spectrum of the Fe [CSC]ii[/CSC]–Rich Broad Absorption Line QSO IRAS 07598+6508". The Astrophysical Journal. 448 (2). doi:10.1086/309611. ISSN 0004-637X.
  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.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  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.
  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?". The Astrophysical Journal. doi:10.1086/343075/fulltext/56010.text.html#tb4. Retrieved 2024-10-06.
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