Wikipedia

SBSS 0953+549

SBSS 0953+549 also known as SBS 0953+549 and QSO J0957+5440, is a quasar located in the constellation of Ursa Major. With a redshift of 2.58, the object is located 10.8 billion light-years away from Earth.[1] It is a broad absorption-line quasar (BAL QSO) according to Sloan Digital Sky Survey.[2]

SBSS 0953+549
SBSS 0953+549 captured by SDSS
Observation data (J2000.0 epoch)
ConstellationUrsa Major
Right ascension09h 57m 14.67s
Declination+54d 40m 17.53s
Redshift2.589463
Heliocentric radial velocity776,302 km/s
Distance10.843 Gly (light travel time distance)
Apparent magnitude (V)0.018
Apparent magnitude (B)0.023
Surface brightness17.4
Characteristics
TypeHiBAL
Other designations
2MASS J09571464+5440179, PGC 4052729, SDSS J095714.67+544017.5, SBS 0953+549, NRRF J095714.6+544018, KODIAQ J095714+544017, QSO J0957+5440

Characteristics

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First observed by the Second Byurakan Survey aiming to reach faint limiting magnitudes for stellar objects in 1986,[3][4] SBSS 0953+549 is classified as a luminous quasar with a bolometric luminosity correction of relative 2500 Å of BC2500 Å =2.75 ± 0.40 according to researchers using the integrated light technique from 1 μm-2 keV via mid-infrared data from Spitzer and Wide-field Infrared Survey Explorer (WISE), near-infrared data from the Two Micron All Sky Survey and UKIDSS, optical data from the Sloan Digital Sky Survey, and ultraviolet data from the Galaxy Evolution Explorer.[5]

Specifically containing high-ionization troughs relative to the quasar's rest frame, SBSS 0953+549 has redshifted troughs that extends high to velocities up to v ≃ 12 000 km s−1 with its trough widths exceed 3000 km s−1.[6] According to Hall, the quasar is found to have absorption from C IV λλ1548, 1550 at all observed wavelengths in Å, N V λλ1238, 1242 and O VI λλ1031, 1037, and considered herby, the most common subtype of BAL QSOs.[7] Such BAL troughs like in SBSS 0953+549 is found to have a wide range of velocities that is relative to the quasar, both collectively and in individual objects. The traditional velocity range over which the strength of BAL troughs detected in C IV λλ1548, 1550 is evaluated is −25 000 to −3000 km s−1.[8] Furthermore, SBSS 0953+549 contains a Lyman-alpha emission-line profile is similar to P Cygni with line profiles which are observed in the spectra of stars with expanding shells.[4]

In addition, SBSS 0953+549 is also an X-ray emitting active galaxy according to observations by ROSAT[9] containing damped Ly-alpha absorbers (DLAs), defined as absorbers with HI column density N(HI) >= 1020.3 cm−2, impling an incidence per absorption length, l(X)= 0.017(+0.014-0.008) at a median survey path redshift of z=0.623 and a HI mass density at z ~ 0.6 of rho_HI = 0.25(+0.20-0.12) x 108 Msol Mpc−3[10] at the velocity separation δv<3000 km/s from the quasar.[11]

Observations

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Researchers who studied the broad emission-line profiles in SBSS 0953+549 involving correlations with line width, found new strong trends. As line width at FWHM increases, the ratio of line peak to continuum intensity decreases for C III λ1909 while the intensity ratio C III λ1909/C IV λ1549 increases. The intensity ratio of C III] λ1909/Mg II λ2798 decreases as well, while peaks of C III] λ1909 and C IV λ1549 become increasingly blueshifted relative to the Mg II λ2798 peak. This proves SBSS 0953+549 is a radio-quiet object with broader C III λ1909 and C IV λ1549 lines than objects classified as radio-loud, but distributions of Mg II FWHMs do not differ. As for the average ratio of the broad emission-line profiles in SBSS 0953+539, it is <FWHM_C III]_/FWHM_Mg II_> = 1.59 +/- 0.08 and <FWHM_C IV_/FWHM_Mg II_> = 1.35 +/- 0.09. According to researchers, the quasar is found to have a narrow core (FWHM ~2000 km s−1) and a broad base (FWHM ~7000 km s−1) blueshifted by ~1000 km s−1 meaning it has a smaller core-to-base ratio.[12]

Apart from that, researchers also found a sample of Lyman-alpha forest lines in the spectra of SBSS 0953+549 whom they studied it for the proximity effect. According to them calculating the column density distribution, through an effective velocity dispersion parameter, from the observed equivalent width distribution, they found the background intensity value is reduced by a factor of 2 to 3 making it three times smaller compared the values obtained from the whole sample, thus confirming the presence of dust in such damped Lyalpha systems like in SBSS 0953+549.[13]

Amongst many quasar observed by researchers using archival Hubble Space Telescope observations with the Faint Object Spectrograph and Space Telescope Imaging Spectrograph, they were able to identify at least 206 optically thick Lyman limit systems (LLSs) at z < 2.6 located within the vicinity of SBSS 0953+549. Looking through the incidence of such LLSs per redshift unit, l(z) = dn/dz, at these redshifts is well described by a single power law, l(z)vprop(1 + z)γ. These systems are located over the redshift range 0.2 <= z <= 4.9, with γ = 1.33 ± 0.61 at z < 2.6, or with γ = 1.83 ± 0.21 . The incidence of LLSs per absorption distance, l(X), decreases by a factor of ~1.5 over the ~0.6 Gyr from z = 4.9 to 3.5; l(X) but evolves more slowly at low redshifts decreasing by a similar factor over the ~8 Gyr from z = 2.6 to 0.25.[14]

Mg II and C IV absorption systems

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SBSS 0953+549 contains a number Mg II absorption systems discovered at 1.98 <= z <= 5.33 in the infrared spectra. According to researchers, all the Mg II systems are either to be of damped Lyα absorbers (DLAs) or sub-DLAs, with 40.7% of systems exceeding the DLA threshold that is compared to 16.7% at \bar{z} = 0.927. They are mostly classical systems (W λ2796 0 = 0.3-1.0 Å), preferentially associated with sub-DLAs, that are quite metal rich at ~0.1 solar.[15]

They also performed an analysis of 34,000 Mg II doublets at 0.36 < z < 2.29, and found 50% completeness at rest equivalent width of W r ≈ 0.8 Å. These Mg II doublets are equivalent with width frequency distribution described by an exponential model at all redshifts, making the distribution becoming flatter as redshift increases; there are more strong systems relative to weak ones. Moreover, they found the estimated physical cross-section of MgII-absorbing galaxy halos increased by three-fold, from z = 0.4 --> 2.3, while the W_r >= 1 Angstrom absorber line density grew, dN_MgII/dX, by roughly 45%.[16]

Besides Mg II absorbers, researchers found 16,000 C IV systems with 1.46 < z < 4.55. According to researchers, they found the co-moving line density of dN_CIV/dX has evolved with the redshift, increasing by a factor of 2.37+/-0.09 from z = 4.55 to 1.96 before stabilizing at dN_CIV/dX ~ 0.34 for z = 1.96 to 1.46. Comparing the SDSS sample with z < 1 (ultraviolet) and z > 5 (infrared) surveys, researchers see an approximately 10-fold increase in dN_CIV/dX over z ~ 6 --> 0, for W_r >= 0.6 Å suggesting significant increase in the enrichment of gas outside galaxies over the 12 Gyr lifetime of the universe.[17]

Host galaxy

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The host galaxy of SBSS 0954+549 is a massive early-type galaxy[18] surround by circumgalactic medium (CGM) with a massive dark matter halo measuring 1012 M ⊙. Looking at the scale of the virial radius (r vir ≈ 160 kpc), they measured a high covering fraction fC = 0.73 ± 0.10 to strong C II 1334 absorption (rest equivalent width W 1334 >= 0.2 Å), implying a massive reservoir of cool (T ~ 104 K) metal enriched gas in SBSS 0954+549.[19] In addition, the host galaxy has a co-moving volume density of 0.0135+/-0.00550.0035 Mpc−3 and has ongoing star formations, creating new stellar populations with an average rate of 50 M⊙ yr−1 as observed from the Hα flux, making it a starburst galaxy.[20]

Emission-line protogalaxy candidate

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Through narrow-band infrared imaging, researchers found a faint red galaxy with a strong (equivalent width = 2%) emission line at 2.30 mu m. This field was observed due to the proximity to the quasar SBSS 0953+549, which contains a metal-line absorption system at zabs = 2.50. The emission-line galaxy is only found separated from the quasar line of sight with a projected distance of 240 kpc. Researchers identified the emission line as H alpha /[N II] in a galaxy found in the same group as the z = 2.50 absorber. Since all the galaxy properties are also consistent with a young age and a redshift of 2.5, it is a protogalaxy candidate.[21]

Galaxy companions

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Besides the emission-line galaxy, researchers found two new galaxies lying at redshifts of z ~ 0.1. They are found to be progenitors of luminous field galaxies of ~ 3 x 1011 M_sun, in which they found the upper limits to and the detection of carbon oxide emission from these distant galaxies are consistent with the suggested upper limit to galaxy masses of 10(12) M_sun as posed by the cooling time argument.[22]

Not only they were able to find the two new galaxies, they were able to narrowband infrared imaging to discover an H alpha emitting galaxy at a redshift of z = 2.5. Through optical spectroscopy with the Keck-I telescope reveals a spectrum of both strong narrow emission lines, especially Ly alpha and the stellar and interstellar absorption lines that the characteristics of young starbursts, at a redshift of 2.498. This galaxy has a current star formation rate of 10–100 Msolar yr−1,with the burst of star formation starting no earlier than z ~ 5.5. According to researchers, it should evolve into a normal galaxy of present-day luminosity of L* or less making a protogalaxy. Furthermore, they found two close pairs of fainter H alpha -emitting galaxies lying within 500 kpc of the first galaxy, containing H alpha luminosities and bluer colors, whom they propose these three galaxies are members of young galaxy cluster at z = 2.5.[23]

References

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  1. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-06-23.
  2. ^ Trump, Jonathan R.; Hall, Patrick B.; Reichard, Timothy A.; Richards, Gordon T.; Schneider, Donald P.; Vanden Berk, Daniel E.; Knapp, Gillian R.; Anderson, Scott F.; Fan, Xiaohui; Brinkman, J.; Kleinman, S. J.; Nitta, Atsuko (2006-07-01). "A Catalog of Broad Absorption Line Quasars from the Sloan Digital Sky Survey Third Data Release". The Astrophysical Journal Supplement Series. 165 (1): 1–18. arXiv:astro-ph/0603070. Bibcode:2006ApJS..165....1T. doi:10.1086/503834. ISSN 0067-0049.
  3. ^ Stepanian, J. A. (2005-04-01). "The Second Byurakan Survey. General Catalogue". Revista Mexicana de Astronomia y Astrofisica. 41: 155–368. Bibcode:2005RMxAA..41..155S. ISSN 0185-1101.
  4. ^ a b Levshakov, S. A.; Varshalovich, D. A.; Nazarov, E. A. (1986-11-01). "Spectral study of quasars from the Second Byurakan Survey of the north hemisphere. I. The quasars SBS 0953+549, SBS 1116+603 and SBS 1138+584". Astrofizika. 25: 495–506. Bibcode:1986Afz....25..495L.
  5. ^ Krawczyk, Coleman M.; Richards, Gordon T.; Mehta, Sajjan S.; Vogeley, Michael S.; Gallagher, S. C.; Leighly, Karen M.; Ross, Nicholas P.; Schneider, Donald P. (2013-05-01). "Mean Spectral Energy Distributions and Bolometric Corrections for Luminous Quasars". The Astrophysical Journal Supplement Series. 206 (1): 4. arXiv:1304.5573. Bibcode:2013ApJS..206....4K. doi:10.1088/0067-0049/206/1/4. ISSN 0067-0049.
  6. ^ Hall, P. B.; Brandt, W. N.; Petitjean, P.; Pâris, I.; Filiz Ak, N.; Shen, Yue; Gibson, R. R.; Aubourg, É.; Anderson, S. F.; Schneider, D. P.; Bizyaev, D.; Brinkmann, J.; Malanushenko, E.; Malanushenko, V.; Myers, A. D. (2013-07-13). "Broad absorption line quasars with redshifted troughs: high-velocity infall or rotationally dominated outflows?". Monthly Notices of the Royal Astronomical Society. 434 (1): 222–256. arXiv:1306.2680. doi:10.1093/mnras/stt1012. ISSN 0035-8711.
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  13. ^ Srianand, R.; Khare, Pushpa (1996-06-01). "Analysis of Lyalpha absorption lines in the vicinity of QSOs". Monthly Notices of the Royal Astronomical Society. 280 (3): 767–780. arXiv:astro-ph/9511048. Bibcode:1996MNRAS.280..767S. doi:10.1093/mnras/280.3.767. ISSN 0035-8711.
  14. ^ Ribaudo, Joseph; Lehner, Nicolas; Howk, J. Christopher (2011-07-01). "A Hubble Space Telescope Study of Lyman Limit Systems: Census and Evolution". The Astrophysical Journal. 736 (1): 42. arXiv:1105.0659. Bibcode:2011ApJ...736...42R. doi:10.1088/0004-637X/736/1/42. ISSN 0004-637X.
  15. ^ Matejek, Michael S.; Simcoe, Robert A.; Cooksey, Kathy L.; Seyffert, Eduardo N. (2013-02-01). "Mg II Absorption at 2 < z < 6 with Magellan/FIRE. II. A Longitudinal Study of H I, Metals, and Ionization in Galactic Halos". The Astrophysical Journal. 764 (1): 9. arXiv:1207.2470. Bibcode:2013ApJ...764....9M. doi:10.1088/0004-637X/764/1/9. ISSN 0004-637X.
  16. ^ Seyffert, Eduardo N.; Cooksey, Kathy L.; Simcoe, Robert A.; O'Meara, John M.; Kao, Melodie M.; Prochaska, J. Xavier (2013-12-03). "Precious Metals in SDSS Quasar Spectra II: Tracking the Evolution of Strong, 0.4 < z < 2.3 MgII Absorbers with Thousands of Systems". The Astrophysical Journal. 779 (2): 161. arXiv:1308.5971. Bibcode:2013ApJ...779..161S. doi:10.1088/0004-637X/779/2/161. ISSN 0004-637X.
  17. ^ Cooksey, Kathy L.; Kao, Melodie M.; Simcoe, Robert A.; O'Meara, John M.; Prochaska, J. Xavier (2013-01-20). "Precious Metals in SDSS Quasar Spectra I: Tracking the Evolution of Strong, 1.5 < z < 4.5 CIV Absorbers with Thousands of Systems". The Astrophysical Journal. 763 (1): 37. arXiv:1204.2827. Bibcode:2013ApJ...763...37C. doi:10.1088/0004-637X/763/1/37. ISSN 0004-637X.
  18. ^ Lupi, Alessandro; Volonteri, Marta; Decarli, Roberto; Bovino, Stefano; Silk, Joseph; Bergeron, Jacqueline (2019-09-01). "High-redshift quasars and their host galaxies - I. Kinematical and dynamical properties and their tracers". Monthly Notices of the Royal Astronomical Society. 488 (3): 4004–4022. arXiv:1901.02464. Bibcode:2019MNRAS.488.4004L. doi:10.1093/mnras/stz1959. ISSN 0035-8711.
  19. ^ Prochaska, J. Xavier; Lau, Marie Wingyee; Hennawi, Joseph F. (2014-12-01). "Quasars Probing Quasars. VII. The Pinnacle of the Cool Circumgalactic Medium Surrounds Massive z ~ 2 Galaxies". The Astrophysical Journal. 796 (2): 140. arXiv:1409.6344. Bibcode:2014ApJ...796..140P. doi:10.1088/0004-637X/796/2/140. ISSN 0004-637X.
  20. ^ Teplitz, Harry I.; Malkan, M.; McLean, I. S. (1998-10-01). "An Infrared Search for Star-forming Galaxies at Z > 2". The Astrophysical Journal. 506 (2): 519–532. arXiv:astro-ph/9805157. Bibcode:1998ApJ...506..519T. doi:10.1086/306255. ISSN 0004-637X.
  21. ^ Malkan, M.; Teplitz, H.; McLean, I. (1995-07-01). "An Emission-Line Protogalaxy Candidate at z=2.5". The Astrophysical Journal. 448: L5. Bibcode:1995ApJ...448L...5M. doi:10.1086/309595. ISSN 0004-637X.
  22. ^ Lo, K. -Y.; Chen, H. -W.; Ho, P. T. P. (1999-01-01). "A survey of molecular gas content of galaxies at 0.08 < Z". Astronomy and Astrophysics. 341: 348–354. Bibcode:1999A&A...341..348L. ISSN 0004-6361.
  23. ^ Malkan, M. A.; Teplitz, H.; McLean, I. S. (1996-09-01). "A Young Cluster of Galaxies at z=2.5". The Astrophysical Journal. 468: L9. Bibcode:1996ApJ...468L...9M. doi:10.1086/310228. ISSN 0004-637X.
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