Astronomy:Markarian 876
| Markarian 876 | |
|---|---|
 HST image of Markarian 876. | |
| Observation data (J2000.0 epoch) | |
| Constellation | Draco |
| Right ascension | 16h 13m 57.17s |
| Declination | +65° 43′ 09.98″ |
| Redshift | 0.121090 |
| Helio radial velocity | 36,302 km/s |
| Distance | 1.752 Gly (537.16 Mpc) |
| Apparent magnitude (V) | 15.49 |
| Apparent magnitude (B) | 16.03 |
| Characteristics | |
| Type | E2, Sy1 |
| Size | 117.72 kiloparsecs (384,000 light-years) (diameter; 2MASS K-band total isophote)[1] |
| Other designations | |
| PGC 57553, PG 1613+658, IRAS 16136+6550, RBS 1567, 2E 3624, 2MASX J16135722+6543096 | |
Markarian 876 (Mrk 876) known as PG 1613+658, is an elliptical galaxy located in the constellation of Draco. With a velocity relative to the cosmic microwave background of 36,302 ± 60 kilometers per seconds, the galaxy is located 1.75 billion light years from Earth. It is a Seyfert galaxy.[1]
Characteristics
Markarian 876 is classified as a large galaxy with a distorted morphology. It has tidal tails extending out from the galaxy by more than 50 arcsecs or 85 kiloparsecs (kpc). The structure of the galaxy appears lopsided and complicated with a secondary nucleus or knot of light located 1.6 arcsec west of the main nucleus.[2] A barred spiral galaxy companion is found lying at the same redshift, indicating the peculiar structure in Markarian 876 might be directly caused by a strong gravitational interaction with the object.[3] However the companion galaxy is located 23 arcsecs north and doesn't seem to tidally connect with Markarian 876, therefore the latter's distorted morphology is likely caused by a galaxy merger.[2]
The mass of the black hole in the center of Markarian 876 is estimated to be (2.2 ± 1.0) x 108 Mʘ based on an optical reverberation campaign.[4]
An emission line is found connected with the source of the galaxy with a rest-frame energy of 4.80+0.05-0.04 keV.[5]
References
- ↑ 1.0 1.1 "By Name NASA/IPAC Extragalactic Database". https://ned.ipac.caltech.edu/byname?objname=MRK+876&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1.
- ↑ 2.0 2.1 Hutchings, J. B.; Neff, S. G. (July 1992). "Optical imaging of QSOs with 0.5 arcsec resolution". The Astronomical Journal 104 (1): 1. doi:10.1086/116216. ISSN 0004-6256. Bibcode: 1992AJ....104....1H.
- ↑ Alloin, D.; Barvainis, R.; Gordon, M.A.; Antonucci, R.R.J. (1992). "CO emission from radio quiet quasars - New detections support a thermal origin for the FIR emission". Astronomy & Astrophysics 265 (2): 429–436. ISSN 0004-6361. Bibcode: 1992A&A...265..429A.
- ↑ Landt, Hermine; Mitchell, Jake A. J.; Ward, Martin J.; Mercatoris, Paul; Pott, Jörg-Uwe; Horne, Keith; Hernández Santisteban, Juan V.; Malhotra, Daksh et al. (March 2023). "A Complex Dust Morphology in the High-luminosity AGN Mrk 876". The Astrophysical Journal 945 (1): 62. doi:10.3847/1538-4357/acb92d. ISSN 0004-637X. Bibcode: 2023ApJ...945...62L.
- ↑ Bottacini, Eugenio; Orlando, Elena; Greiner, Jochen; Ajello, Marco; Moskalenko, Igor; Persic, Massimo (17 December 2014). "An extreme gravitationally redshifted iron line at 4.8 KeV in Mrk 876". The Astrophysical Journal 798 (1): L14. doi:10.1088/2041-8205/798/1/L14. ISSN 2041-8213.
External links
- Markarian 876 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
- Mrk 876 on SIMBAD
 |  |
