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Title: NuSTARUnveils a Compton-Thick Type 2 Quasar in MrK 34

Abstract

We present Nuclear Spectroscopic Telescope Array (NuSTAR) 3-40 keV observations of the optically selected Type 2 quasar (QSO2) SDSS J1034+6001 or Mrk 34. The high-quality hard X-ray spectrum and archival XMM-Newton data can be fitted self-consistently with a reflection-dominated continuum and a strong Fe Kα fluorescence line with equivalent width >1 keV. Prior X-ray spectral fitting below 10 keV showed the source to be consistent with being obscured by Compton-thin column densities of gas along the line of sight, despite evidence for much higher columns from multiwavelength data. NuSTAR now enables a direct measurement of this column and shows that N H lies in the Compton-thick (CT) regime. The new data also show a high intrinsic 2-10 keV luminosity of L 2-10 ~ 1044 erg s–1, in contrast to previous low-energy X-ray measurements where L 2-10 ≲ 1043 erg s–1 (i.e., X-ray selection below 10 keV does not pick up this source as an intrinsically luminous obscured quasar). Both the obscuring column and the intrinsic power are about an order of magnitude (or more) larger than inferred from pre-NuSTAR X-ray spectral fitting. Mrk 34 is thus a "gold standard" CT QSO2 and is the nearest non-merging system in this class,more » in contrast to the other local CT quasar NGC 6240, which is currently undergoing a major merger coupled with strong star formation. For typical X-ray bolometric correction factors, the accretion luminosity of Mrk 34 is high enough to potentially power the total infrared luminosity. In conclusion, X-ray spectral fitting also shows that thermal emission related to star formation is unlikely to drive the observed bright soft component below ~3 keV, favoring photoionization instead.« less

Authors:
ORCiD logo [1];  [1];  [1]; ORCiD logo [2];  [3];  [4];  [2];  [5];  [6];  [7];  [8];  [9];  [10];  [11];  [1];  [12];  [13];  [14];  [2];  [15] more »;  [16];  [17];  [18];  [19];  [20];  [21];  [20];  [17];  [2];  [20] « less
+ Show Author Affiliations
  1. Durham Univ., Durham (United Kingdom)
  2. California Inst. of Technology (CalTech), Pasadena, CA (United States)
  3. Pontificia Univ. Catolica de Chile, Santiago (Chile); Univ. de Valparaiso, Valparaiso (Chile)
  4. Georgia Inst. of Technology, Atlanta, GA (United States)
  5. Pontificia Univ. Catolica de Chile, Santiago (Chile); Space Science Institute, Boulder, CO (United States)
  6. Univ. of California, Berkeley, CA (United States)
  7. The Pennsylvania State Univ., University Park, PA (United States)
  8. Max-Planck-Institut fur extraterrestrische Physik, Garching bei Munchen (Germany)
  9. Technical Univ. of Denmark, Lyngby (Denmark)
  10. INAF Osservatorio Astronomico di Bologna, Bologna (Italy)
  11. Technical Univ. of Denmark, Lyngby (Denmark); Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
  12. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
  13. Institute of Astronomy, Cambridge (United Kingdom)
  14. Columbia Univ., New York, NY (United States)
  15. Dartmouth College, Hanover, NH (United States)
  16. ETH Zurich, Zurich (Switzerland)
  17. Yale Univ., New Haven, CT (United States)
  18. Univ. of California, Berkeley, CA (United States); The Pennsylvania State Univ., University Park, PA (United States)
  19. Stanford Univ., Stanford, CA (United States)
  20. NASA Goddard Space Flight Center (GSFC), Greenbelt, MD (United States)
  21. ASDC-ASI, Roma (Italy); INAF-Osservatorio Astronomico di Roma, Monte Porzio Catone (RM) (Italy)
Publication Date:
Research Org.:
SLAC National Accelerator Lab., Menlo Park, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC); National Aeronautics and Space Administration (NASA)
OSTI Identifier:
1165904
Report Number(s):
SLAC-PUB-16155
Journal ID: ISSN 1538-4357; arXiv:1407.1844
Grant/Contract Number:  
AC02-76SF00515
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 792; Journal Issue: 2; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Astrophysics; ASTRO; GRQC; galaxies: active; X-rays: galaxies; X-rays: individual (Mrk 34)

Citation Formats

Gandhi, P., Lansbury, G. B., Alexander, D. M., Stern, D., Arevalo, P., Ballantyne, D. R., Baloković, M., Bauer, F. E., Boggs, S. E., Brandt, W. N., Brightman, M., Christensen, F. E., Comastri, A., Craig, W. W., Del Moro, A., Elvis, M., Fabian, A. C., Hailey, C. J., Harrison, F. A., Hickox, R. C., Koss, M., LaMassa, S. M., Luo, B., Madejski, G. M., Ptak, A. F., Puccetti, S., Teng, S. H., Urry, C. M., Walton, D. J., and Zhang, W. W. NuSTARUnveils a Compton-Thick Type 2 Quasar in MrK 34. United States: N. p., 2014. Web. doi:10.1088/0004-637X/792/2/117.
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Gandhi, P., Lansbury, G. B., Alexander, D. M., Stern, D., Arevalo, P., Ballantyne, D. R., Baloković, M., Bauer, F. E., Boggs, S. E., Brandt, W. N., Brightman, M., Christensen, F. E., Comastri, A., Craig, W. W., Del Moro, A., Elvis, M., Fabian, A. C., Hailey, C. J., Harrison, F. A., Hickox, R. C., Koss, M., LaMassa, S. M., Luo, B., Madejski, G. M., Ptak, A. F., Puccetti, S., Teng, S. H., Urry, C. M., Walton, D. J., & Zhang, W. W. NuSTARUnveils a Compton-Thick Type 2 Quasar in MrK 34. United States. https://doi.org/10.1088/0004-637X/792/2/117
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Gandhi, P., Lansbury, G. B., Alexander, D. M., Stern, D., Arevalo, P., Ballantyne, D. R., Baloković, M., Bauer, F. E., Boggs, S. E., Brandt, W. N., Brightman, M., Christensen, F. E., Comastri, A., Craig, W. W., Del Moro, A., Elvis, M., Fabian, A. C., Hailey, C. J., Harrison, F. A., Hickox, R. C., Koss, M., LaMassa, S. M., Luo, B., Madejski, G. M., Ptak, A. F., Puccetti, S., Teng, S. H., Urry, C. M., Walton, D. J., and Zhang, W. W. Fri . "NuSTARUnveils a Compton-Thick Type 2 Quasar in MrK 34". United States. https://doi.org/10.1088/0004-637X/792/2/117. https://www.osti.gov/servlets/purl/1165904.
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@article{osti_1165904,
title = {NuSTARUnveils a Compton-Thick Type 2 Quasar in MrK 34},
author = {Gandhi, P. and Lansbury, G. B. and Alexander, D. M. and Stern, D. and Arevalo, P. and Ballantyne, D. R. and Baloković, M. and Bauer, F. E. and Boggs, S. E. and Brandt, W. N. and Brightman, M. and Christensen, F. E. and Comastri, A. and Craig, W. W. and Del Moro, A. and Elvis, M. and Fabian, A. C. and Hailey, C. J. and Harrison, F. A. and Hickox, R. C. and Koss, M. and LaMassa, S. M. and Luo, B. and Madejski, G. M. and Ptak, A. F. and Puccetti, S. and Teng, S. H. and Urry, C. M. and Walton, D. J. and Zhang, W. W.},
abstractNote = {We present Nuclear Spectroscopic Telescope Array (NuSTAR) 3-40 keV observations of the optically selected Type 2 quasar (QSO2) SDSS J1034+6001 or Mrk 34. The high-quality hard X-ray spectrum and archival XMM-Newton data can be fitted self-consistently with a reflection-dominated continuum and a strong Fe Kα fluorescence line with equivalent width >1 keV. Prior X-ray spectral fitting below 10 keV showed the source to be consistent with being obscured by Compton-thin column densities of gas along the line of sight, despite evidence for much higher columns from multiwavelength data. NuSTAR now enables a direct measurement of this column and shows that N H lies in the Compton-thick (CT) regime. The new data also show a high intrinsic 2-10 keV luminosity of L 2-10 ~ 1044 erg s–1, in contrast to previous low-energy X-ray measurements where L 2-10 ≲ 1043 erg s–1 (i.e., X-ray selection below 10 keV does not pick up this source as an intrinsically luminous obscured quasar). Both the obscuring column and the intrinsic power are about an order of magnitude (or more) larger than inferred from pre-NuSTAR X-ray spectral fitting. Mrk 34 is thus a "gold standard" CT QSO2 and is the nearest non-merging system in this class, in contrast to the other local CT quasar NGC 6240, which is currently undergoing a major merger coupled with strong star formation. For typical X-ray bolometric correction factors, the accretion luminosity of Mrk 34 is high enough to potentially power the total infrared luminosity. In conclusion, X-ray spectral fitting also shows that thermal emission related to star formation is unlikely to drive the observed bright soft component below ~3 keV, favoring photoionization instead.},
doi = {10.1088/0004-637X/792/2/117},
journal = {The Astrophysical Journal (Online)},
number = 2,
volume = 792,
place = {United States},
year = {Fri Aug 22 00:00:00 EDT 2014},
month = {Fri Aug 22 00:00:00 EDT 2014}
}
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