1ES 1741+196
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| 1ES 1741+196 | |
|---|---|
 The BL Lac object 1ES 1741+196. | |
| Observation data (J2000.0 epoch) | |
| Constellation | Hercules |
| Right ascension | 17h 43m 57.83s |
| Declination | +19° 35′ 09.01″ |
| Redshift | 0.084000 |
| Heliocentric radial velocity | 25,183 km/s |
| Distance | 1.217 Gly (373.13 Mpc) |
| Apparent magnitude (V) | 16.8 |
| Characteristics | |
| Type | BL Lac |
| Size | 103.65 kiloparsecs (338,100 light-years) (diameter; 2MASS K-band total isophote)[1] |
| Notable features | Low luminosity blazar |
| Other designations | |
| LEDA 1597986, 87GB 174148.7+193615, TXS 1741+196, RX J1743.8+1935, IRCF J174357.8+193509, S3 1741+19, TeV J1743+196 | |
1ES 1741+196 is a BL Lacertae object (BL Lac) located in the constellation of Hercules. It is located 1.2 billion light years from Earth.[1] It was first discovered in 1996 via an Einstein Observatory X-ray satellite.[2][3] Because the galaxy's synchrotron peak is found above 1 keV, it is categorized as a high-frequency peaked object.[4]
The nucleus of 1ES 1741+196 is active. It has been classified as an extreme blazar due to having a flat high energy gamma ray spectrum[5] or alternatively, a high-energy BL Lac.[6] One accepted theory for this energy source in most active galactic nuclei is a presence of an accretion disk around its supermassive black hole. The mass of the black hole in the center of the galaxy is estimated to be 8.93 ± 0.70 M☉ based on a fundamental plane measurement.[7]
Apart from that, 1ES 1741+196 has an isotopic luminosity of ~ 8.2 × 1043 erg s−1, making it less luminous amongst other TeV blazars.[8] When observed in very high energy (VHE) band, 1ES 1741+196 shows no evidence of strong flares.[4] Its X-ray spectrum is known to be variable compared to its steady gamma ray spectrum, with it rising up by a factor of 3 in terms of variability.[5]
The host galaxy of 1ES 1741+196 is an elliptical galaxy, one of the largest and brightest BL Lac host galaxies observed. It has a redshift magnitude relation of -24.85 and a galaxy effective radius of 51.2 kiloparsecs, which its overall luminosity distribution is obtained via a de Vaucouleurs profile. Additionally, there are two galaxy companions within the galaxy's position.[9] They have same redshifts,[10] with projected distances of 7.2 and 25.2 kiloparsecs.[9] Given 1ES 1741+196 has a flat luminosity profile, its position along an impact parameter towards the neighbors and a high ellipticity, this suggests tidal forces. Further evidence also shows a presence of a tidal tail between the companions, indicating the three galaxies are interacting.[9]
1ES 1741+196 has an extended radio jet towards the east direction with a projected position angle of °80.[11][12] The jet is known to be straight despite showing signs of a 5° bend towards south by 15-20 parsecs from its core.[13] Furthermore, the jet is known to be aligned well with a parsec-scale jet.[12]
References
- 1 2 "By Name NASA/IPAC Extragalactic Database". ned.ipac.caltech.edu. Retrieved 2024-10-18.
- ↑ "Astronomers measure and model a blazing gamma-ray source – Astronomy Now". Retrieved 2024-10-18.
- ↑ Perlman, Eric S.; Stocke, John T.; Schachter, Jonathan F.; Elvis, Martin; Ellingson, Erica; Urry, C. Megan; Potter, Michael; Impey, Chris D.; Kolchinsky, Peter (June 1996). "The Einstein Slew Survey Sample of BL Lacertae Objects". The Astrophysical Journal Supplement Series. 104: 251. Bibcode:1996ApJS..104..251P. doi:10.1086/192300. ISSN 0067-0049.
- 1 2 Abeysekara, A.U.; Archambault, S.; Archer, A.; Benbow, W.; Bird, R.; Biteau, J. (May 2016). "VERITAS and multiwavelength observations of the BL Lacertae object 1ES 1741+196". Monthly Notices of the Royal Astronomical Society. 459 (3): 2550–2557. arXiv:1603.07286. doi:10.1093/mnras/stw664.
- 1 2 Goswami, P.; Zacharias, M.; Zech, A.; Chandra, S.; Boettcher, M.; Sushch, I. (February 2024). "The variety of extreme blazars in the AstroSat view" (PDF). Astronomy & Astrophysics. 682: A134. arXiv:2311.12695. Bibcode:2024A&A...682A.134G. doi:10.1051/0004-6361/202348121. ISSN 0004-6361.
- ↑ Lister, Matthew. "MOJAVE Sample: 1741+196". www.cv.nrao.edu. Retrieved 2024-10-18.
- ↑ Vovk, Ie.; Neronov, A. (April 2013). "Variability of Gamma-Ray Emission from Blazars on Black Hole Timescales". The Astrophysical Journal. 767 (103): 103. arXiv:1304.0915. Bibcode:2013ApJ...767..103V. doi:10.1088/0004-637X/767/2/103.
- ↑ Ahnen, M.L.; Ansoldi, S.; Antonelli, L.A.; Antoranz, P.; Arcaro, C.; Babic, A.; Banerjee, B. (June 2017). "MAGIC detection of very high energy γ-ray emission from the low-luminosity blazar 1ES 1741+196". Monthly Notices of the Royal Astronomical Society. 468 (2): 1534–1541. arXiv:1702.06795. doi:10.1093/mnras/stx472.
- 1 2 3 Heidt, J.; Nilsson, K.; Fried, J. W.; Takalo, L. O.; Sillanpää, A. (1999-08-01). "1ES 1741+196: a BL Lacertae object in a triplet of interacting galaxies?". Astronomy and Astrophysics. 348: 113–116. arXiv:astro-ph/9906129. Bibcode:1999A&A...348..113H. ISSN 0004-6361.
- ↑ Nilsson, K.; Pursimo, T.; Heidt, J.; Takalo, L. O.; Sillanpää, A.; Brinkmann, W. (2003-02-24). "R-band imaging of the host galaxies of RGB BL Lacertae objects" (PDF). Astronomy & Astrophysics. 400 (1): 95–118. Bibcode:2003A&A...400...95N. doi:10.1051/0004-6361:20021861. ISSN 0004-6361.
- ↑ Wu, Zhongzu; Jiang, D. R.; Gu, Minfeng; Liu, Yi (2007-02-20). "VLBI observations of seven BL Lacertae objects from RGB sample" (PDF). Astronomy & Astrophysics. 466 (1): 63–73. arXiv:0706.0191. Bibcode:2007A&A...466...63W. doi:10.1051/0004-6361:20066754. ISSN 0004-6361.
- 1 2 Rector, T.A.; Gabuzda, D.C.; Peterson, D.C.; Stocke, J.T. (2005). "The Propagation of Jets in High-Energy Peaked BL Lacertae Objects". Future Directions in High Resolution Astronomy: The 10th Anniversary of the VLBA, ASP Conference Proceedings. 340: 116–118. Bibcode:2005ASPC..340..116R.
- ↑ Rector, Travis A.; Gabuzda, Denise C.; Stocke, John T. (March 2003). "The Radio Structure of High-Energy–Peaked BL Lacertae Objects". The Astronomical Journal. 125 (3): 1060–1072. arXiv:astro-ph/0302397. Bibcode:2003AJ....125.1060R. doi:10.1086/367802. ISSN 0004-6256.
