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Multiwavelength morphological study of active galaxies

Published online by Cambridge University Press:  29 January 2021

Betelehem Bilata-Woldeyes ,
Mirjana Pović ,
Zeleke Beyoro-Amado ,
Tilahun Getachew-Woreta  and
Shimeles Terefe
Betelehem Bilata-Woldeyes
Affiliation:
Debre Berhan University (DBU), Debre Berhan, Ethiopia Ethiopian Space Science and Technology Institute (ESSTI), Addis Ababa, Ethiopia
Mirjana Pović
Affiliation:
Ethiopian Space Science and Technology Institute (ESSTI), Addis Ababa, Ethiopia Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain
Zeleke Beyoro-Amado
Affiliation:
Ethiopian Space Science and Technology Institute (ESSTI), Addis Ababa, Ethiopia
Tilahun Getachew-Woreta
Affiliation:
Ethiopian Space Science and Technology Institute (ESSTI), Addis Ababa, Ethiopia
Shimeles Terefe
Affiliation:
Ethiopian Space Science and Technology Institute (ESSTI), Addis Ababa, Ethiopia
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Abstract

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Studying the morphology of a large sample of active galaxies at different wavelengths and comparing it with active galactic nuclei (AGN) properties, such as black hole mass (MBH) and Eddington ratio (λEdd), can help us in understanding better the connection between AGN and their host galaxies and the role of nuclear activity in galaxy formation and evolution. By using the BAT-SWIFT hard X-ray public data and by extracting those parameters measured for AGN and by using other public catalogues for parameters such as stellar mass (M*), star formation rate (SFR), bolometric luminosity (Lbol), etc., we studied the multiwavelength morphological properties of host galaxies of ultra-hard X-ray detected AGN and their correlation with other AGN properties. We found that ultra hard X-ray detected AGN can be hosted by all morphological types, but in larger fractions (42%) they seem to be hosted by spirals in optical, to be quiet in radio, and to have compact morphologies in X-rays. When comparing morphologies with other galaxy properties, we found that ultra hard X-ray detected AGN follow previously obtained relations. On the SFR vs. stellar mass diagram, we found that although the majority of sources are located below the main sequence (MS) of star formation (SF), still non-negligible number of sources, with diverse morphologies, is located on and/or above the MS, suggesting that AGN feedback might have more complex influence on the SF in galaxies than simply quenching it, as it was suggested in some of previous studies.

Keywords

active galaxiesmorphologymultiwavelength studystar formation rate
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S356: Nuclear Activity in Galaxies Across Cosmic Time , October 2019 , pp. 295 - 298
Copyright
© The Author(s), 2021. Published by Cambridge University Press on behalf of International Astronomical Union

References

Baumgartner, W. H. et al. 2013, ApJS, 207, 19 Google Scholar
Brinchmann, J. & Ellis, R. S. 2000, ApJ, 536, L77 CrossRefGoogle Scholar
Conselice, C. J., 2014, Annu. Rev. Astron. Astrophys, 52, 291 CrossRefGoogle Scholar
Elbaz, D. et al. 2007, A&A, 468, 33 Google Scholar
Fanidakis, N. et al. 2010, MNRAS, 410, 53 CrossRefGoogle Scholar
Gabor, J. M. et al. 2009, ApJ, 691, 705 10.1088/0004-637X/691/1/705CrossRefGoogle Scholar
Hickox, R. C. et al. 2009, ApJ, 696, 891 Google Scholar
Ho, L. C., 2008, Annu. Rev. Astron. Astrophys., 46, 475 CrossRefGoogle Scholar
Kauffmann, G. et al. 2003, MNRAS, 346, 1055 10.1111/j.1365-2966.2003.07154.xCrossRefGoogle Scholar
Koss, M. et al. 2011, ApJ, 739, 57 Google Scholar
Koss, M. et al. 2017, ApJ, 850, 74 10.3847/1538-4357/aa8ec9CrossRefGoogle Scholar
Leslie, S. K. et al. 2016, MNRAS, 455, L82 Google Scholar
Poggianti, B. M. et al. 2008, ApJ, 684, 888 CrossRefGoogle Scholar
Pović, M., et al. 2009a, ApJ, 706, 810 10.1088/0004-637X/706/1/810CrossRefGoogle Scholar
Pović, M. et al. 2009b, ApJ, 702, L51 10.1088/0004-637X/702/1/L51CrossRefGoogle Scholar
Pović, M. et al. 2012, A&A, 541, A118 Google Scholar
Ricci, C. et al. 2017, arXiv preprint arXiv:1709.03989Google Scholar
Schawinski, K. et al. 2010, ApJ, 711, 284 CrossRefGoogle Scholar