CTQ 327
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| CTQ 327 | |
|---|---|
 DSS image of CTQ 327. | |
| Observation data (J2000.0 epoch) | |
| Constellation | Hydra |
| Right ascension | 13h 55m 43.43s |
| Declination | −22° 57′ 23.16″ |
| Redshift | 1.370000 |
| Heliocentric radial velocity | 410,716 km/s |
| Distance | 8.735 Gly |
| Apparent magnitude (B) | +18.2 |
| Characteristics | |
| Type | QSO |
| Other designations | |
| 2MASSI J1355434-225723, 2CXO J135543.4-225723, CTS 0327, CTS M15.16 | |
CTQ 327 also known as Q 1355-2257, is a gravitationally-lensed quasar located in the constellation of Hydra. It was discovered in 1992 from the Calan-Tololo Survey,[1] with its redshift of the object calculated as (z) 1.37 by N.D. Morgan during the Hubble Space Telescope Imaging Spectrograph snapshot survey in August 2003.[2]
CTQ 327 is a double imaged quasar.[3][4] When imaged by Morgan, the object is found to separate into two bright images or components, with an estimated separation gap of 1.22 arcseconds and a g-band flux ratio roughly 5 to 1. The components are found to display continuum and emission line features in their spectra, mainly doubly ionized carbon and magnesium, despite not similar to one another, with component A having much weaker emission lines compared to component B.[2][5][6]
The lensing galaxy of CTQ 327 is resolved and classified an early-type elliptical galaxy with a redshift of (z) 0.70, located from component B by 0.29 milliarcseconds.[2][7] An absorption feature is found to be associated with it at (z) 0.48.[8] A stellar mass of 11.56 M☉, and an effective radius of 1.24 ± 0.29 arcseconds has been found for the lens galaxy with the total Einstein radius of 0.62 arcseconds.[9]
The quasar displays time-delays. Based on observations by P. Saha using a lens model, the predicted time-delay is −89+28−39 days long.[6] A more recent study in August 2020, estimated a new time-delay of −81.5+10.8−12.0 days based on a measurement pipeline.[10] It is shown the flux ratios of both components have temporal variations based on g-band Magellan observations of 0.14 magnitude during a period of over three months. Comparison of second-epoch data obtained in March and June, have also found component A of CTQ 327 underwent a significant decrease in brightness by 0.125 ± 0.001 magnitude while component B showed no observed changes.[2]
CTQ 327 has evidence of chromatic microlensing with wavelengths greater than λ > 6180Å. Astronomers also noted, the core of emission lines and continuum also displayed a discrepancy in magnitude results of -0.06 and +0.08 respectively. They also noted the accretion disk of CTQ 327 is larger with a size of 3.6+3.0−1.6 x 1.3 ± 0.6 M/M☉ and has a temperature profile of 2.0 ± 0.7. The black hole mass is estimated as 1.1 × 109 M☉.[11]
References
- ↑ Maza, J.; Ruiz, M. T.; Gonzalez, L. E.; Wischnjewsky, M.; Antezana, R. (April 1993). "Calan-Tololo Survey. V. Two hundred new southern quasars". Revista Mexicana de Astronomía y Astrofísica. 25: 51–57. Bibcode:1993RMxAA..25...51M. ISSN 0185-1101.
- 1 2 3 4 Morgan, N. D.; Gregg, M. D.; Wisotzki, L.; Becker, R.; Maza, J.; Schechter, P. L.; White, R. L. (August 2003). "CTQ 327: A New Gravitational Lens". The Astronomical Journal. 126 (2): 696–705. Bibcode:2003AJ....126..696M. doi:10.1086/376470. ISSN 0004-6256.
- ↑ Morgan, Nicholas D. (2002). "New optical surveys for gravitationally lensed quasars". Ph.D. Thesis: 1287. Bibcode:2002PhDT........29M.
- ↑ 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.
- ↑ Fian, C.; Mediavilla, E.; Motta, V.; Jiménez-Vicente, J.; Muñoz, J. A.; Chelouche, D.; Hanslmeier, A. (2021-09-01). "Microlensing of the broad emission lines in 27 gravitationally lensed quasars - Broad line region structure and kinematics" (PDF). Astronomy & Astrophysics. 653: A109. arXiv:2107.06227. Bibcode:2021A&A...653A.109F. doi:10.1051/0004-6361/202039829. ISSN 0004-6361.
- 1 2 Saha, P.; Courbin, F.; Sluse, D.; Dye, S.; Meylan, G. (2006-05-01). "COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses - IV. Models of prospective time-delay lenses" (PDF). Astronomy & Astrophysics. 450 (2): 461–469. arXiv:astro-ph/0601370. Bibcode:2006A&A...450..461S. doi:10.1051/0004-6361:20052929. ISSN 0004-6361.
- ↑ Eigenbrod, A.; Courbin, F.; Meylan, G.; Vuissoz, C.; Magain, P. (2006-06-01). "COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses - III. Redshift of the lensing galaxy in eight gravitationally lensed quasars" (PDF). Astronomy & Astrophysics. 451 (3): 759–766. arXiv:astro-ph/0511026. Bibcode:2006A&A...451..759E. doi:10.1051/0004-6361:20054454. ISSN 0004-6361.
- ↑ Ofek, Eran O.; Maoz, Dan; Rix, Hans-Walter; Kochanek, Christopher S.; Falco, Emilio E. (April 2006). "Spectroscopic Redshifts for Seven Lens Galaxies". The Astrophysical Journal. 641 (1): 70–77. arXiv:astro-ph/0510465. Bibcode:2006ApJ...641...70O. doi:10.1086/500403. ISSN 0004-637X.
- ↑ Oguri, Masamune; Rusu, Cristian E.; Falco, Emilio E. (April 2014). "The stellar and dark matter distributions in elliptical galaxies from the ensemble of strong gravitational lenses". Monthly Notices of the Royal Astronomical Society. 439 (3): 2494–2504. arXiv:1309.5408. doi:10.1093/mnras/stu106. ISSN 0035-8711.
- ↑ Millon, M.; Courbin, F.; Bonvin, V.; Paic, E.; Meylan, G.; Tewes, M.; Sluse, D.; Magain, P.; Chan, J. H. H.; Galan, A.; Joseph, R.; Lemon, C.; Tihhonova, O.; Anderson, R. I.; Marmier, M. (2020-08-01). "COSMOGRAIL - XIX. Time delays in 18 strongly lensed quasars from 15 years of optical monitoring". Astronomy & Astrophysics. 640: A105. arXiv:2002.05736. Bibcode:2020A&A...640A.105M. doi:10.1051/0004-6361/202037740. ISSN 0004-6361.
- ↑ Rojas, K.; Motta, V.; Mediavilla, E.; Jiménez-Vicente, J.; Falco, E.; Fian, C. (2020-02-06). "Microlensing Analysis for the Gravitational Lens Systems SDSS0924+0219, Q1355-2257, and SDSS1029+2623". The Astrophysical Journal. 890 (1): 3. arXiv:2002.02861. Bibcode:2020ApJ...890....3R. doi:10.3847/1538-4357/ab63cb. ISSN 0004-637X.
