Astronomy:PKS 1538+149

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PKS 1538+149
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Sloan Digital Sky Survey image of PKS 1538+149.
Observation data (J2000.0 epoch)
ConstellationSerpens
Right ascension 15h 40m 49.49s
Declination+14° 47′ 45.88″
Redshift0.606441
Helio radial velocity181,806 km/s
Distance5.733 Gly
Apparent magnitude (V)17.30
Apparent magnitude (B)17.72
Characteristics
TypeOpt. var; FRSQ BLLAC
Other designations
4C +14.60, MG J1540+1447, LEDA 2819234, OR +165, CoNFIG 226, Cul 1538+149, RX J1540.8+1447, 2MASSI J1540494+144745, SDSS J154049.49+144745.8

PKS 1538+149 also known as 4C 14.60, is a BL Lacertae object[1] located in the constellation of Serpens. The redshift of the object is found to be (z) 0.605[2] and was discovered through photoelectric observations in February 1975 by astronomers who observed it had a continuous spectra.[3] The radio spectrum of the source is flat, describing it a flat-spectrum radio quasar (FRSQ).[4]

Description

PKS 1538+149 is shown undergoing a decrease in brightness levels by displaying a low visual magnitude of 1.7 as observed by E.R. Craine and K. Johnson.[3] It is noted to be variable too, when it was detected by J.T. Pollock in 1975, who noted the object had an amplitude exceeding more than a magnitude of 2.8 ± 0.20, however it has no evidence of variations in X-ray flux.[5][6] During the period between April and June 1986, the light curve data, showed it undergoing a decrease of 0.0026 magnitude per day, averaging on the magnitude of 18.54.[7] The object is also classified as a blazar due to its high optical polarization, displaying large variations more than 1 magnitude while the spectral index described as both steep and also variable, remained constant.[8][9][10]

The radio structure of PKS 1538+149 is described as compact. On arcsecond scales, the source has a size of 6 centimeters with radio emission depicted as being concentrated in its northern region.[11] Observations also showed the source is elongated with radio frequency identification imaging finding the emission further extends northwest by 60 milliarcseconds and by 10 milliarcseconds at 8.4 GHz frequencies.[12] It is found PKS 1538+149 has a jet with jet power of 2.36 x 1045 ergs with an opening angle of 16.1°. The radio core is noted shifting by 0.032 milliarcseconds in frequencies of 8.1-15.3 GHz.[13]

Earlier observations, especially using near-infrared H-band found PKS 1538+149 has an unresolved host galaxy.[14] Imaging with Hubble Space Telescope would later reveal the host galaxy is indeed a round elliptical galaxy, surrounded by several other faint galaxies within its vicinity. It has a low surface brightness and V-I color of 2.85. A de Vaucouleurs model also described the host galaxy as large and luminous with a measured magnitude of -25.1 and length of 21 kilometers in size.[15] A central supermassive black hole mass of 7.54 x 104 Mʘ was found for the object.[4]

References

  1. ↑ Falomo, R.; Treves, A.; Chiappetti, L.; Maraschi, L.; Pian, E.; Tanzi, E. G. (January 1993). "The Ultraviolet--to--Near-Infrared Spectral Flux Distribution of Four BL Lacertae Objects" (in en). The Astrophysical Journal 402: 532. doi:10.1086/172154. ISSN 0004-637X. Bibcode: 1993ApJ...402..532F. https://articles.adsabs.harvard.edu/pdf/1993ApJ...402..532F. 
  2. ↑ Kotilainen, J. K.; Hyvönen, T.; Falomo, R. (2005-09-01). "The luminous host galaxies of high redshift BL Lac objects" (in en). Astronomy & Astrophysics 440 (3): 831–843. doi:10.1051/0004-6361:20042548. ISSN 0004-6361. Bibcode: 2005A&A...440..831K. https://www.aanda.org/articles/aa/pdf/2005/36/aa2548-04.pdf. 
  3. ↑ 3.0 3.1 Craine, E. R.; Johnson, K.; Tapia, S. (February 1975). "UBVr sequences and observations of optically identified radio sources." (in en). Publications of the Astronomical Society of the Pacific 87: 123–130. doi:10.1086/129733. ISSN 0004-6280. Bibcode: 1975PASP...87..123C. https://articles.adsabs.harvard.edu/pdf/1975PASP...87..123C. 
  4. ↑ 4.0 4.1 Xie, Guang-Zhong; Chen, Luo-En; Li, Huai-Zhen; Mao, Li-Sheng; Dai, Hong; Xie, Zhao-Hua; Ma, Li; Zhou, Shu-Bai (October 2005). "Estimates of AGN Black Hole Mass and Minimum Variability Timescale". Chinese Journal of Astronomy and Astrophysics 5 (5): 463–470. doi:10.1088/1009-9271/5/5/004. ISSN 1009-9271. Bibcode: 2005ChJAA...5..463X. https://iopscience.iop.org/article/10.1088/1009-9271/5/5/004/pdf. 
  5. ↑ Pollock, J. T. (June 1975). "Variability and optical-radio properties of BL Lacertae objects". The Astrophysical Journal 198: L53. doi:10.1086/181809. ISSN 0004-637X. Bibcode: 1975ApJ...198L..53P. https://articles.adsabs.harvard.edu//full/1975ApJ...198L..53P/L000053.000.html. 
  6. ↑ Maccagni, D.; Tarenghi, M. (January 1981). "X-ray observations of six BL Lacertae fields." (in en). The Astrophysical Journal 243: 42–46. doi:10.1086/158564. ISSN 0004-637X. Bibcode: 1981ApJ...243...42M. https://articles.adsabs.harvard.edu/pdf/1981ApJ...243...42M. 
  7. ↑ Kidger, Mark R. (October 1988). "CCD monitoring of quasars and BL Lacertae objects". Publications of the Astronomical Society of the Pacific 100: 1248. doi:10.1086/132311. ISSN 0004-6280. Bibcode: 1988PASP..100.1248K. https://iopscience.iop.org/article/10.1086/132311/pdf. 
  8. ↑ Rusk, R. E.; Seaquist, E. R.; Yen, J. L. (September 1983). "Polarized Compact Radio Sources" (in en). Bulletin of the American Astronomical Society 15: 957. Bibcode: 1983BAAS...15..957R. https://articles.adsabs.harvard.edu/pdf/1983BAAS...15..957R. 
  9. ↑ Falomo, R.; Scarpa, R.; Bersanelli, M. (July 1994). "Optical Spectrophotometry of Blazars" (in en). The Astrophysical Journal Supplement Series 93: 125. doi:10.1086/192048. ISSN 0067-0049. Bibcode: 1994ApJS...93..125F. https://articles.adsabs.harvard.edu/pdf/1994ApJS...93..125F. 
  10. ↑ Impey, C. D.; Brand, P. W. J. L.; Wolstencroft, R. D.; Williams, P. M. (July 1984). "Infrared polarimetry and photometry of BL Lac objects - II." (in en). Monthly Notices of the Royal Astronomical Society 209 (2): 245–269. doi:10.1093/mnras/209.2.245. ISSN 0035-8711. https://articles.adsabs.harvard.edu/pdf/1984MNRAS.209..245I. 
  11. ↑ Ulvestad, J. S.; Johnston, K. J.; Weiler, K. W. (March 1983). "The arc second radio structure of 12 BL Lacertae objects". The Astrophysical Journal 266: 18. doi:10.1086/160755. ISSN 0004-637X. Bibcode: 1983ApJ...266...18U. https://adsabs.harvard.edu/full/1983ApJ...266...18U. 
  12. ↑ Zensus, J. A.; Ros, E.; Kellermann, K. I.; Cohen, M. H.; Vermeulen, R. C.; Kadler, M. (August 2002). "Sub-milliarcsecond Imaging of Quasars and Active Galactic Nuclei. II. Additional Sources" (in en). The Astronomical Journal 124 (2): 662–674. doi:10.1086/341585. ISSN 0004-6256. Bibcode: 2002AJ....124..662Z. 
  13. ↑ Nokhrina, E. E.; Beskin, V. S.; Kovalev, Y. Y.; Zheltoukhov, A. A. (March 2015). "Intrinsic physical conditions and structure of relativistic jets in active galactic nuclei" (in en). Monthly Notices of the Royal Astronomical Society 447 (3): 2726–2737. doi:10.1093/mnras/stu2587. ISSN 0035-8711. 
  14. ↑ Kotilainen, Jari K.; Falomo, Renato; Scarpa, Riccardo (August 1998). "The host galaxies of BL Lac objects in the near-infrared" (in en). Astronomy and Astrophysics 336: 479–489. ISSN 0004-6361. Bibcode: 1998A&A...336..479K. 
  15. ↑ Urry, C. Megan; Falomo, Renato; Scarpa, Riccardo; Pesce, Joseph E.; Treves, Aldo; Giavalisco, Mauro (February 1999). "Hubble Space Telescope Observations of the Host Galaxies of BL Lacertae Objects" (in en). The Astrophysical Journal 512 (1): 88–99. doi:10.1086/306763. ISSN 0004-637X. Bibcode: 1999ApJ...512...88U. 



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