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Probing the building blocks of galaxies: Sub-galactic scaling relations between X-ray luminosity, SFR and stellar mass

Published online by Cambridge University Press:  10 June 2020

K. Kouroumpatzakis Open the ORCID record for K. Kouroumpatzakis [Opens in a new window] ,
A. Zezas Open the ORCID record for A. Zezas [Opens in a new window] ,
P. H. Sell Open the ORCID record for P. H. Sell [Opens in a new window] ,
P. Bonfini Open the ORCID record for P. Bonfini [Opens in a new window] ,
M. L. N. Ashby Open the ORCID record for M. L. N. Ashby [Opens in a new window]  and
S. P. Willner Open the ORCID record for S. P. Willner [Opens in a new window]
K. Kouroumpatzakis
Affiliation:
Department of Physics, University of Crete, GR-70013 Heraklion, Greece email: [email protected] Institute of Astrophysics, FORTH, GR-71110 Heraklion, Greece
A. Zezas
Affiliation:
Department of Physics, University of Crete, GR-70013 Heraklion, Greece email: [email protected] Institute of Astrophysics, FORTH, GR-71110 Heraklion, Greece Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA
P. H. Sell
Affiliation:
Department of Physics, University of Crete, GR-70013 Heraklion, Greece email: [email protected] Institute of Astrophysics, FORTH, GR-71110 Heraklion, Greece
P. Bonfini
Affiliation:
Department of Physics, University of Crete, GR-70013 Heraklion, Greece email: [email protected] Institute of Astrophysics, FORTH, GR-71110 Heraklion, Greece
M. L. N. Ashby
Affiliation:
Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA
S. P. Willner
Affiliation:
Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA
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Abstract

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It is well known that X-ray luminosity (Lx) originating from high mass X-ray binaries (HMXBs) is tightly correlated with the host galaxy’s star formation rate (SFR). We explore this connection using a sample representative of the star-formation activity in the local Universe (Star-Formation Reference Survey; SFRS) along with a comprehensive set of star-formation (radio, FIR, 24μm, 8 μm, Hα, UV, SED fitting) and stellar mass (K-band, 3.6 μm, SED fitting) indicators, and Chandra observations. We investigate the Lx–SFR and Lx– stellar mass (M*) scaling relations down to sub-galactic scales of ∼lkpc2. This way we extend these relations to extremely low SFR (∼10−6M⊙.yr−1) and M* (∼104M⊙). We also quantify their scatter and their dependence on the age of the local stellar populations as inferred from the different age sensitive SFR indicators. These results are particularly important for setting the benchmark for the formation of X-ray binaries in vigorous, but low SFR objects such as galaxies in the early Universe.

Keywords

galaxies:star formationX-rays: galaxiesX-rays:binaries
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S341: Challenges in Panchromatic Modelling with Next Generation Facilities , November 2019 , pp. 162 - 166
Copyright
© International Astronomical Union 2020

References

Ashby, M., Mahajan, S., Smith, H. A., Willner, S. P., Fazio, G. G., Raychaudhury, S., Zezas, A., Barmby, P., et al. 2011, PASP, 123, 90710.1086/661920CrossRefGoogle Scholar
Boquien, M., Buat, V., Perret, V., et al. 2014, A&A, 571, A72Google Scholar
Cervino, M., Bongiovanni, A., Hidalgo, S., et al. 2016, A&A, 589, A108Google Scholar
Douna, V. M., Pellizza, L. J., Mirabel, I. F., Pedrosa, S. E., et al. 2015, A&A, 579, A44Google Scholar
Fragos, T., Lehmer, B., Tremmel, M., Tzanavaris, P., Basu-Zych, A., Belczynski, K., Hornschemeier, A., Jenkins, L., et al. 2013, AJ, 764, 1Google Scholar
Gilfanov, M. 2004, MNRAS, 349, 110.1111/j.1365-2966.2004.07473.xCrossRefGoogle Scholar
Lehmer, B. D., Basu-Zych, A. R., Mineo, S., Brandt, W. N., Eufrasio, R. T., Fragos, T., Hornschemeier, A. E., Luo, B., et al. 2016, AJ, 825, 1Google Scholar
Maragkoudakis, A., Zezas, A., Ashby, M. L. N., Willner, S. P., et al. 2017, MNRAS, 475, 2Google Scholar
Mineo, S., Gilfanov, M., Sunyaev, R., et al. 2012, AJ, 737, 2Google Scholar
Mineo, S., Gilfanov, M., Lehmer, B. D., Morrison, G. E., Sunyaev, R., et al. 2014, MNRAS, 437, 210.1093/mnras/stt1999CrossRefGoogle Scholar
Murphy, E. J., Condon, J. J., Schinnerer, E., Kennicutt, R. C., Calzetti, D., Armus, L., Helou, G., Turner, J. L., et al. 2011, MNRAS, 419, 3Google Scholar
Park, T., Kashyap, V. L., Siemiginowska, A., van Dyk, D. A., Zezas, A., Heinke, C., Wargelin, B. J., et al. 2006, AJ, 652, 1Google Scholar
Sell, P., Zezas, A., Kouroumpatzakis, K., Bonfini, P., Ashby, M., Willner, S., et al. 2019, In preparationGoogle Scholar