HE 2149-2745

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HE 2149-2745
HE 2149-2745 DSS.jpg
Gravationally lensed quasar HE 2149-2745, as taken with DSS.
Observation data (J2000.0 epoch)
Constellation Piscis Austrinus
Right ascension 21h 52m 07.40s
Declination −27° 31′ 49.00″
Redshift 2.033000
Heliocentric radial velocity 609,478 km/s
Distance 10.103 Gly
Apparent magnitude  (V)18.39
Apparent magnitude  (B)18.70
Characteristics
Type QSO
Other designations
QSO B2149-2745, 2MASS J21520747-2731497, 2QZ J215207.4-273150, QSO B2149-275, TIC 53893830, PGC 4023719

HE 2149-2745 is a strong gravitationally lensed quasar located in the southern constellation of Piscis Austrinus. It has a redshift of (z) 2.033 [1] and was first discovered by astronomers in 1996. It is also classified as a broad absorption line (BAL) quasar as it shows absorption lines in its spectrum. [2] [3] [4]

Contents

Description

HE 2149-2745 is classified as a double quasar. When imaged, it is separated into two components with a separation gap of 1.7 arcseconds and each having B magnitudes of 17.3 and 19.0 respectively. The components also display P Cygni type emission or absorption profiles but found indistinguishable from one another. [2] The lens galaxy of HE 2149-2745 is classified as an elliptical galaxy according to observations by Sebastian Lopez who estimated its redshift between (z) 0.3 and (z) 0.5. [5] [6] A spectroscopic result by A. Eigenbrod would later confirm the galaxy's redshift as (z) 0.603 although a redshift of (z) 0.495 is suggested. [7] [8] [3] The lens mass of the galaxy is estimated to be 1.5(2.4) x 1011 Mʘ with an R magnitude of 20.4. [9] It is also suggested the lens galaxy might be part of a cluster given there are several other galaxies in R-band imaging. [3]

The quasar displays time-delays. Based on results using the V-band light curve data obtained via the 1.5 meter telescope at La Silla Observatory, the time-delays are estimated as 103 ± 12 days, [4] while dismissing later time-delay estimates of either 70–85 days or 100–110 days when observed by Eva Eulaers and Pierre Magain. [10] Observations also found the A and B components have marginal differences of 1.635 ± 0.001 and 1.505 ± 0.003 magnitudes in both V and I-bands. Evidence points out the A component is much bluer than the B component, but the color differences doesn't vary in both components during the observation period. [4] In addition, HE 2149-2745 displays some variations in its flux ratio showing fluctuations at 0.03 suggesting microlensing variability. [11]

The broad-line region of HE 2149-2745 is observed. When studied by astronomers, the accretion disk size is found to be measured as 8+11-5 M/Mʘ light-days. An estimate of the size vs. wavelength exponent was calculated as 0.4 ± 0.3. [12] Microlensing of its broad-line region is suggested, given evidence of absorbed doubly ionized carbon emission caused by time-variable absorption in both components. [13] A supermassive black hole mass of 9.31 ± 0.93 Mʘ has been found for the quasar. [14]

References

  1. ↑ "NED search results for HE 2149-2745". NASA/IPAC Extragalactic Database. Retrieved 2025-06-21.
  2. 1 2 Wisotzki, L.; Koehler, T.; Lopez, S.; Reimers, D. (November 1996). "Discovery of a new gravitationally lensed QSO with broad absorption lines". Astronomy and Astrophysics. 315: 405–408. Bibcode:1996A&A...315L.405W. ISSN   0004-6361.
  3. 1 2 3 Momcheva, Ivelina G.; Williams, Kurtis A.; Cool, Richard J.; Keeton, Charles R.; Zabludoff, Ann I. (2015-08-17). "A Spectroscopic Survey of the Fields of 28 Strong Gravitational Lenses". The Astrophysical Journal Supplement Series. 219 (2): 29. arXiv: 1503.02074 . Bibcode:2015ApJS..219...29M. doi:10.1088/0067-0049/219/2/29. ISSN   1538-4365.
  4. 1 2 3 Burud, I.; Courbin, F.; Magain, P.; Lidman, C.; Hutsemékers, D.; Kneib, J.-P.; Hjorth, J.; Brewer, J.; Pompei, E.; Germany, L.; Pritchard, J.; Jaunsen, A. O.; Letawe, G.; Meylan, G. (2002-02-01). "An optical time-delay for the lensed BAL quasar HE 2149-2745". Astronomy & Astrophysics. 383 (1): 71–81. arXiv: astro-ph/0112225 . Bibcode:2002A&A...383...71B. doi:10.1051/0004-6361:20011731. ISSN   0004-6361.
  5. ↑ Lopez, Sebastian; Wucknitz, Olaf; Wisotzki, Lutz (1998-09-14), "Detection of the lensing galaxy in HE 2149-2745", Astronomy and Astrophysics, 339, arXiv: astro-ph/9809170 , Bibcode:1998A&A...339L..13L, arXiv:astro-ph/9809170
  6. ↑ Sluse, D.; Chantry, V.; Magain, P.; Courbin, F.; Meylan, G. (2012-02-01). "COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses - X. Modeling based on high-precision astrometry of a sample of 25 lensed quasars: consequences for ellipticity, shear, and astrometric anomalies". Astronomy & Astrophysics. 538: A99. arXiv: 1112.0005 . Bibcode:2012A&A...538A..99S. doi:10.1051/0004-6361/201015844. ISSN   0004-6361.
  7. ↑ Sorgenfrei, C.; Schmidt, R. W.; Wambsganss, J. (March 2024). "Improving the light curves of gravitationally lensed quasars with Gaia proper motion data". Astronomy & Astrophysics. 683: A119. arXiv: 2401.10071 . Bibcode:2024A&A...683A.119S. doi:10.1051/0004-6361/202347381. ISSN   0004-6361.
  8. ↑ Eigenbrod, A.; Courbin, F.; Meylan, G. (2007-04-01). "COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses - VI. Redshift of the lensing galaxy in seven gravitationally lensed quasars" (PDF). Astronomy & Astrophysics. 465 (1): 51–56. arXiv: astro-ph/0612419 . Bibcode:2007A&A...465...51E. doi:10.1051/0004-6361:20066939. ISSN   0004-6361.
  9. ↑ Faure, C.; Alloin, D.; Kneib, J. P.; Courbin, F. (2004-12-01). "A search for clusters and groups of galaxies on the line of sight towards 8 lensed quasars" (PDF). Astronomy & Astrophysics. 428 (3): 741–755. arXiv: astro-ph/0405521 . Bibcode:2004A&A...428..741F. doi:10.1051/0004-6361:20040406. ISSN   0004-6361.
  10. ↑ Eulaers, Eva; Magain, Pierre (2011-12-23), "Time delays for eleven gravitationally lensed quasars revisited", Astronomy & Astrophysics, 536: A44, arXiv: 1112.2609 , Bibcode:2011A&A...536A..44E, doi:10.1051/0004-6361/201016101
  11. ↑ Fadely, Ross; Keeton, Charles R. (2011-02-11). "Near-infrared K and L Flux Ratios in Six Lensed Quasars". The Astronomical Journal. 141 (3): 101. arXiv: 1101.1917 . Bibcode:2011AJ....141..101F. doi:10.1088/0004-6256/141/3/101. ISSN   0004-6256.
  12. ↑ Motta, V.; Mediavilla, E.; Rojas, K.; Falco, E. E.; Jiménez-Vicente, J.; Muñoz, J. A. (February 2017). "Probing the Broad-Line Region and the Accretion Disk in the Lensed Quasars HE 0435-1223, WFI 2033-4723, and HE 2149-2745 Using Gravitational Microlensing". The Astrophysical Journal. 835 (2): 132. arXiv: 1703.00400 . Bibcode:2017ApJ...835..132M. doi: 10.3847/1538-4357/835/2/132 . ISSN   0004-637X.
  13. ↑ Sluse, D.; Hutsemékers, D.; Courbin, F.; Meylan, G.; Wambsganss, J. (2012-08-01). "Microlensing of the broad line region in 17 lensed quasars". Astronomy & Astrophysics. 544: A62. arXiv: 1206.0731 . Bibcode:2012A&A...544A..62S. doi:10.1051/0004-6361/201219125. ISSN   0004-6361.
  14. ↑ Melo, A.; Motta, V.; Mejía-Restrepo, J.; Assef, R. J.; Godoy, N.; Mediavilla, E.; Falco, E.; Kochanek, C. S.; Ávila-Vera, F.; Jerez, R. (December 2023). "Black hole masses for 14 gravitationally lensed quasars". Astronomy and Astrophysics. 680: A51. arXiv: 2306.03472 . Bibcode:2023A&A...680A..51M. doi:10.1051/0004-6361/202347078. ISSN   0004-6361.
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