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== Characteristics ==
== Characteristics ==
SDSS J135646.10+102609.0 is a merger product between two [[Interacting galaxy|colliding galaxies]], namely a [[Disc galaxy|disk galaxy]] and an [[elliptical galaxy]].<ref name=":0">{{Cite journal |last=Sun |first=Ai-Lei |last2=Greene |first2=Jenny E. |last3=Zakamska |first3=Nadia L. |last4=Nesvadba |first4=Nicole P. H. |date=2014-08-01 |title=ALMA Observations of a Candidate Molecular Outflow in an Obscured Quasar |url=https://ui.adsabs.harvard.edu/abs/2014ApJ...790..160S/abstract |journal=The Astrophysical Journal |volume=790 |pages=160 |doi=10.1088/0004-637X/790/2/160 |issn=0004-637X}}</ref><ref>{{Cite web |last=Pierce |first=J C S |last2=Tadhunter |first2=C |last3=Almeida |first3=C Ramos |last4=Bessiere |first4=P |last5=Heaton |first5=J V |last6=Ellison |first6=S L |date=2023-02-23 |title=Galaxy interactions are the dominant trigger for local type 2 quasars |url=https://academic.oup.com/mnras/article/522/2/1736/7035603#403358992 |website=Oxford Academic |series=Monthly Notices of the Royal Astronomical Society |pages=1736-1751 |doi=10.1093/mnras/stad455}}</ref> The galaxy has a luminosity of L<sub>bol</sub> ≈ 10<sup>46</sup> [[erg]] s<sup>-1</sup> with an estimated [[black hole]] mass of M ~ 108 M<sub>Θ</sub>.<ref name=":0" />
SDSS J135646.10+102609.0 is a merger product between two [[Interacting galaxy|colliding galaxies]], namely a [[Disc galaxy|disk galaxy]] and an [[elliptical galaxy]].<ref name=":0">{{Cite journal |last=Sun |first=Ai-Lei |last2=Greene |first2=Jenny E. |last3=Zakamska |first3=Nadia L. |last4=Nesvadba |first4=Nicole P. H. |date=2014-08-01 |title=ALMA Observations of a Candidate Molecular Outflow in an Obscured Quasar |url=https://ui.adsabs.harvard.edu/abs/2014ApJ...790..160S/abstract |journal=The Astrophysical Journal |volume=790 |pages=160 |doi=10.1088/0004-637X/790/2/160 |issn=0004-637X}}</ref><ref>{{Cite web |last=Pierce |first=J C S |last2=Tadhunter |first2=C |last3=Almeida |first3=C Ramos |last4=Bessiere |first4=P |last5=Heaton |first5=J V |last6=Ellison |first6=S L |date=2023-02-23 |title=Galaxy interactions are the dominant trigger for local type 2 quasars |url=https://academic.oup.com/mnras/article/522/2/1736/7035603#403358992 |website=Oxford Academic |series=Monthly Notices of the Royal Astronomical Society |pages=1736-1751 |doi=10.1093/mnras/stad455}}</ref> The galaxy has a luminosity of L<sub>bol</sub> ≈ 10<sup>46</sup> [[erg]] s<sup>-1</sup> with an estimated [[black hole]] mass of M ~ M<sub>Θ</sub>.<ref name=":0" />


SDSS J135646.10+102609.0 has two active nuclei found merging, with a projected separation of only 2.4 or ~ 2.5 [[Parsec|kiloparsecs]].<ref name=":1" /><ref>{{Cite journal |last=Dutta |first=R |last2=Srianand |first2=R |last3=Gupta |first3=N |date=2018-07-17 |title=Prevalence of neutral gas in centres of merging galaxies |url=http://dx.doi.org/10.1093/mnras/sty1872 |journal=Monthly Notices of the Royal Astronomical Society |volume=480 |issue=1 |pages=947–964 |doi=10.1093/mnras/sty1872 |issn=0035-8711}}</ref> While nothing is known about the south nucleus, the north nucleus is classfied a type 2 quasar and is the main galaxy merger member. Its host is a massive [[Elliptical galaxy|early-type galaxy]] or an ETG for short, with a [[position angle]] of 156 degrees. With a [[stellar population]] mainly made up of old [[Star|stars]], the [[Star formation|star formation rate]] of the galaxy derived from infrared luminosity is 69 M<sub>Θ</sub> yr<sup>-1</sup> according to a [[Atacama Large Millimeter Array]] (ALMA) sample. This high star formation rate indicates a consequence of an ongoing merger.<ref name=":1">{{Cite journal |last=Almeida |first=C. Ramos |last2=Bischetti |first2=M. |last3=García-Burillo |first3=S. |last4=Alonso-Herrero |first4=A. |last5=Audibert |first5=A. |last6=Cicone |first6=C. |last7=Feruglio |first7=C. |last8=Tadhunter |first8=C. N. |title=The diverse cold molecular gas contents, morphologies, and kinematics of type-2 quasars as seen by ALMA |url=https://www.aanda.org/articles/aa/full_html/2022/02/aa41906-21/aa41906-21.html#S5 |journal=Astronomy & Astrophysics |volume=658 |page=29 |doi=10.1051/0004-6361/202141906}}</ref>
SDSS J135646.10+102609.0 has two active nuclei found merging, with a projected separation of only 2.4 or ~ 2.5 [[Parsec|kiloparsecs]].<ref name=":1" /><ref>{{Cite journal |last=Dutta |first=R |last2=Srianand |first2=R |last3=Gupta |first3=N |date=2018-07-17 |title=Prevalence of neutral gas in centres of merging galaxies |url=http://dx.doi.org/10.1093/mnras/sty1872 |journal=Monthly Notices of the Royal Astronomical Society |volume=480 |issue=1 |pages=947–964 |doi=10.1093/mnras/sty1872 |issn=0035-8711}}</ref> While nothing is known about the south nucleus, the north nucleus is classfied a type 2 quasar and is the main galaxy merger member. Its host is a massive [[Elliptical galaxy|early-type galaxy]] or an ETG for short, with a [[position angle]] of 156 degrees. With a [[stellar population]] mainly made up of old [[Star|stars]], the [[Star formation|star formation rate]] of the galaxy derived from infrared luminosity is 69 M<sub>Θ</sub> yr<sup>-1</sup> according to a [[Atacama Large Millimeter Array]] (ALMA) sample. This high star formation rate indicates a consequence of an ongoing merger.<ref name=":1">{{Cite journal |last=Almeida |first=C. Ramos |last2=Bischetti |first2=M. |last3=García-Burillo |first3=S. |last4=Alonso-Herrero |first4=A. |last5=Audibert |first5=A. |last6=Cicone |first6=C. |last7=Feruglio |first7=C. |last8=Tadhunter |first8=C. N. |title=The diverse cold molecular gas contents, morphologies, and kinematics of type-2 quasars as seen by ALMA |url=https://www.aanda.org/articles/aa/full_html/2022/02/aa41906-21/aa41906-21.html#S5 |journal=Astronomy & Astrophysics |volume=658 |page=29 |doi=10.1051/0004-6361/202141906}}</ref>

Revision as of 11:24, 22 September 2024

SDSS J135646.10+102609.0
The galaxy merger, SDSS J135646.10+102609.0
Observation data (J2000.0 epoch)
ConstellationBoötes
Right ascension13h 56m 46.10s
Declination+10° 26′ 08.72″
Redshift0.123134
Heliocentric radial velocity36,915 km/s
Distance1.853 Gly (568.1 Mpc)
Apparent magnitude (V)0.10
Apparent magnitude (B)0.13
Characteristics
TypeQSO2
Notable featuresgalaxy merger, luminous infrared galaxy
Other designations
LEDA 1379498, 2MASX J13564607+1026088, IRAS F13543+1040, NVSS J135646+102609, 2CXO J135646.0+102608

SDSS J135646.10+102609.0 known as SDSS J1356+1026 and J1356+1026, is a low redshift quasar and galaxy merger located in the constellation of Boötes. It is located 1.85 billion light years from Earth.[1] It is an ultraluminous inflared galaxy. It is considered radio-quiet with an unresolved radio source.[2]

Characteristics

SDSS J135646.10+102609.0 is a merger product between two colliding galaxies, namely a disk galaxy and an elliptical galaxy.[3][4] The galaxy has a luminosity of Lbol ≈ 1046 erg s-1 with an estimated black hole mass of M ~ 108 MΘ.[3]

SDSS J135646.10+102609.0 has two active nuclei found merging, with a projected separation of only 2.4 or ~ 2.5 kiloparsecs.[5][6] While nothing is known about the south nucleus, the north nucleus is classfied a type 2 quasar and is the main galaxy merger member. Its host is a massive early-type galaxy or an ETG for short, with a position angle of 156 degrees. With a stellar population mainly made up of old stars, the star formation rate of the galaxy derived from infrared luminosity is 69 MΘ yr-1 according to a Atacama Large Millimeter Array (ALMA) sample. This high star formation rate indicates a consequence of an ongoing merger.[5]

The north nucleus is heavily obscured.[3][7] It was originally found during the Sloan Digital Sky Survey[8] based on its [ O III] λ5007 emission.[9][10] The north nucleus also has an average velocity dispersion value of 160 km s-1. According to B-I color map of the galaxy using HST/WFC 3 images, astronomers found a dust lane crossing its nucleus with its position angle matching with the oxocarbon major axis. Using spatial scales, they were able to find the north nucleus has redder optical colors.[5]

In addition, the north nucleus contains a compact rotating disk and an extended tidal arm. Both components contain molecular gas mass of Mmol ≈ 3 x 108 MΘ and Mmol ≈ 5 x 108 MΘ. Further investigations from ALMA also pointed out the tidal arm is the largest molecular tidal feature, implying a small chance of shock dissociation.[3]

Further investigations also shows the presence of soft X-ray emission around the quasar nucleus of SDSS J135646.10+102609.0, extending by 20 kiloparsecs (kpc). This is interpreted as thermal gas with a luminosity of LX ≈ 1042 erg s-1 and temperature of KT ≈ 280 eV. With a faint X-ray luminosity of ~ 10, this suggests the X-ray emission is controlled by either photoionization or shocked emission via a quasar-driven superwind.[11] A study also mentions the superwind driven by the quasar is prototypical.[12]

Galactic outflow

SDSS J135646.10+102609.0 has two symmetric outflows originating from its nucleus. The outflows are measured to be 10 kpc and have observed projected expansion velocities of 250 km s-1. Through a presentation of a kinetic model, the deprojected expansion velocity for this outflows are measured ~ 1000 km-1 with expanding shell kinetic energy of 1044-45 erg s-1.[7]

Star formation

Based on observations from ALMA and oxocarbon observations, a low star formation rate of 16 MΘ yr-1 from far-infrared spectral energy and <16 MΘ yr-1 from the molecular content is found in SDSS J135646.10+102609.0. This suggests the active galactic nucleus of the galaxy is likely responsible for high outflow rate. With an outflowing mass of Mmol ≈ 7 x 107 MΘ, and short dynamical time, the outflow could potentially depleting the gas content inside SDSS J135646.10+102609.0 within few million years.[3]

Double-peaked emission lines

SDSS J135646.10+102609.0 is known to be an interesting system. According to long-slit observations, it contains two [O III] λ5007 emission knots proportional to the two nuclei seen in near-infrared imaging suggesting the double peaks are produced by a dual AGN. However when the extended [O III] emission and nuclei were observed again, this creates a speculation the double peaks are only powered by a single AGN.[13]

References

  1. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-09-20.
  2. ^ Becker, Robert H.; White, Richard L.; Helfand, David J. (1995-09-01). "The FIRST Survey: Faint Images of the Radio Sky at Twenty Centimeters". The Astrophysical Journal. 450: 559. doi:10.1086/176166. ISSN 0004-637X.
  3. ^ a b c d e Sun, Ai-Lei; Greene, Jenny E.; Zakamska, Nadia L.; Nesvadba, Nicole P. H. (2014-08-01). "ALMA Observations of a Candidate Molecular Outflow in an Obscured Quasar". The Astrophysical Journal. 790: 160. doi:10.1088/0004-637X/790/2/160. ISSN 0004-637X.
  4. ^ Pierce, J C S; Tadhunter, C; Almeida, C Ramos; Bessiere, P; Heaton, J V; Ellison, S L (2023-02-23). "Galaxy interactions are the dominant trigger for local type 2 quasars". Oxford Academic. Monthly Notices of the Royal Astronomical Society. pp. 1736–1751. doi:10.1093/mnras/stad455.{{cite web}}: CS1 maint: unflagged free DOI (link)
  5. ^ a b c Almeida, C. Ramos; Bischetti, M.; García-Burillo, S.; Alonso-Herrero, A.; Audibert, A.; Cicone, C.; Feruglio, C.; Tadhunter, C. N. "The diverse cold molecular gas contents, morphologies, and kinematics of type-2 quasars as seen by ALMA". Astronomy & Astrophysics. 658: 29. doi:10.1051/0004-6361/202141906.
  6. ^ Dutta, R; Srianand, R; Gupta, N (2018-07-17). "Prevalence of neutral gas in centres of merging galaxies". Monthly Notices of the Royal Astronomical Society. 480 (1): 947–964. doi:10.1093/mnras/sty1872. ISSN 0035-8711.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  7. ^ a b Greene, Jenny E.; Zakamska, Nadia L.; Smith, Paul S. (2012-02-01). "A Spectacular Outflow in an Obscured Quasar". The Astrophysical Journal. 746: 86. doi:10.1088/0004-637X/746/1/86. ISSN 0004-637X.
  8. ^ York, Donald G.; Adelman, J.; Henderson, John E.; Anderson, Scott F.; Annis, James; Bahcall, Neta A.; Bakken, J. A. "The Sloan Digital Sky Survey: Technical Summary". The Astrophysical Journal. 120 (3). doi:10.1086/301513.
  9. ^ Zakamska, Nadia L.; Strauss, Michael A.; Krolik, Julian H.; Collinge, Matthew J.; Hall, Patrick B; Hao, Lei (November 2002). "Candidate Type II Quasars from the Sloan Digital Sky Survey. I. Selection and Optical Properties of a Sample at 0.3<Z<0.83". The Astrophysical Journal. 126 (5): 2125–2144. arXiv:astro-ph/0309551. Bibcode:2003AJ....126.2125Z. doi:10.48550/arXiv.astro-ph/0309551.
  10. ^ Reyes, Reinabelle; Zakamska, Nadia L.; Strauss, Michael A.; Green, Joshua; Krolik, Julian H.; Shen, Yue; Richards, Gordon T.; Anderson, Scott F. "Space Density of Optically Selected Type 2 Quasars". The Astronomical Journal. 136 (6): 2373–2390. arXiv:0801.1115. doi:10.1088/0004-6256/136/6/2373.
  11. ^ E. Greene, Jenny; Pooley, David; Zakamska, Nadia L.; M. Comerford, Julia. "EXTENDED X-RAY EMISSION FROM A QUASAR-DRIVEN SUPERBUBBLE". The Astrophysical Journal. 788 (54). doi:10.1088/0004-637X/788/1/54.
  12. ^ Somalwar, Jean; Johnson, Sean D.; Stern, Jonathan; Goulding, Andy D.; Greene, Jenny E.; Zakamska, Nadia L.; Alexandroff, Rachael M.; Chen, Hsiao-Wen (2020-02-20). "Spatially Resolved UV Diagnostics of AGN Feedback: Radiation Pressure Dominates in a Prototypical Quasar-driven Superwind". The Astrophysical Journal Letters. 890 (2): L28. doi:10.3847/2041-8213/ab733d. ISSN 2041-8205.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  13. ^ Comerford, Julia M.; Pooley, David; Barrows, R. Scott; Greene, Jenny E.; Zakamska, Nadia L.; Madejski, Greg M.; Cooper, Michael C. (2015-06-19). "MERGER-DRIVEN FUELING OF ACTIVE GALACTIC NUCLEI: SIX DUAL AND OF AGNs DISCOVERED WITHCHANDRAANDHUBBLE SPACE TELESCOPEOBSERVATIONS". The Astrophysical Journal. 806 (2): 219. doi:10.1088/0004-637x/806/2/219. ISSN 1538-4357.
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