NEW INSIGHTS ON THE GALACTIC BULGE INITIAL MASS FUNCTION

A. Calamida, K. C. Sahu, S. Casertano, J. Anderson, S. Cassisi, M. Gennaro, M. Cignoni, T. M. Brown, N. Kains, H. Ferguson, M. Livio, H. E. Bond, R. Buonanno, W. Clarkson, I. Ferraro, A. Pietrinferni, M. Salaris, J. Valenti

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Abstract

We have derived the Galactic bulge initial mass function (IMF) of the Sagittarius Window Eclipsing Extrasolar Planet Search field in the mass range 0.15 < M/M⊙ 1.0, using deep photometry collected with the Advanced Camera for Surveys on the Hubble Space Telescope. Observations at several epochs, spread over 9 years, allowed us to separate the disk and bulge stars down to very faint magnitudes, F814W ≈ 26 mag, with a proper-motion accuracy better than 0.5 mas yr-1 (20 km s-1). This allowed us to determine the IMF of the pure bulge component uncontaminated by disk stars for this low-reddening field in the Sagittarius window. In deriving the mass function, we took into account the presence of unresolved binaries, errors in photometry, distance modulus and reddening, as well as the metallicity dispersion and the uncertainties caused by adopting different theoretical color-temperature relations. We found that the Galactic bulge IMF can be fitted with two power laws with a break at M ∼0.56 M⊙, the slope being steeper (α = -2.41 ± 0.50) for the higher masses, and shallower (α = -1.25 ± 0.20) for the lower masses. In the high-mass range, our derived mass function agrees well with the mass function derived for other regions of the bulge. In the low-mass range however, our mass function is slightly shallower, which suggests that separating the disk and bulge components is particularly important in the low-mass range. The slope of the bulge mass function is also similar to the slope of the mass function derived for the disk in the high-mass regime, but the bulge mass function is slightly steeper in the low-mass regime. We used our new mass function to derive stellar mass-to-light values for the Galactic bulge and we obtained 2.1 < M/ LF814W < 2.4 and 3.1 < M/LF606W < 3.6 according to different assumptions on the slope of the IMF for masses larger than 1M⊙.

Original languageEnglish (US)
Article number8
JournalAstrophysical Journal
Volume810
Issue number1
DOIs
StatePublished - Sep 1 2015

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galactic bulge
slopes
photometry

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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Calamida, A., Sahu, K. C., Casertano, S., Anderson, J., Cassisi, S., Gennaro, M., ... Valenti, J. (2015). NEW INSIGHTS ON THE GALACTIC BULGE INITIAL MASS FUNCTION. Astrophysical Journal, 810(1), [8]. https://doi.org/10.1088/0004-637X/810/1/8
Calamida, A. ; Sahu, K. C. ; Casertano, S. ; Anderson, J. ; Cassisi, S. ; Gennaro, M. ; Cignoni, M. ; Brown, T. M. ; Kains, N. ; Ferguson, H. ; Livio, M. ; Bond, H. E. ; Buonanno, R. ; Clarkson, W. ; Ferraro, I. ; Pietrinferni, A. ; Salaris, M. ; Valenti, J. / NEW INSIGHTS ON THE GALACTIC BULGE INITIAL MASS FUNCTION. In: Astrophysical Journal. 2015 ; Vol. 810, No. 1.
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Calamida, A, Sahu, KC, Casertano, S, Anderson, J, Cassisi, S, Gennaro, M, Cignoni, M, Brown, TM, Kains, N, Ferguson, H, Livio, M, Bond, HE, Buonanno, R, Clarkson, W, Ferraro, I, Pietrinferni, A, Salaris, M & Valenti, J 2015, 'NEW INSIGHTS ON THE GALACTIC BULGE INITIAL MASS FUNCTION', Astrophysical Journal, vol. 810, no. 1, 8. https://doi.org/10.1088/0004-637X/810/1/8

NEW INSIGHTS ON THE GALACTIC BULGE INITIAL MASS FUNCTION. / Calamida, A.; Sahu, K. C.; Casertano, S.; Anderson, J.; Cassisi, S.; Gennaro, M.; Cignoni, M.; Brown, T. M.; Kains, N.; Ferguson, H.; Livio, M.; Bond, H. E.; Buonanno, R.; Clarkson, W.; Ferraro, I.; Pietrinferni, A.; Salaris, M.; Valenti, J.

In: Astrophysical Journal, Vol. 810, No. 1, 8, 01.09.2015.

Research output: Contribution to journalArticle

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AU - Sahu, K. C.

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AU - Cassisi, S.

AU - Gennaro, M.

AU - Cignoni, M.

AU - Brown, T. M.

AU - Kains, N.

AU - Ferguson, H.

AU - Livio, M.

AU - Bond, H. E.

AU - Buonanno, R.

AU - Clarkson, W.

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AU - Salaris, M.

AU - Valenti, J.

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N2 - We have derived the Galactic bulge initial mass function (IMF) of the Sagittarius Window Eclipsing Extrasolar Planet Search field in the mass range 0.15 < M/M⊙ 1.0, using deep photometry collected with the Advanced Camera for Surveys on the Hubble Space Telescope. Observations at several epochs, spread over 9 years, allowed us to separate the disk and bulge stars down to very faint magnitudes, F814W ≈ 26 mag, with a proper-motion accuracy better than 0.5 mas yr-1 (20 km s-1). This allowed us to determine the IMF of the pure bulge component uncontaminated by disk stars for this low-reddening field in the Sagittarius window. In deriving the mass function, we took into account the presence of unresolved binaries, errors in photometry, distance modulus and reddening, as well as the metallicity dispersion and the uncertainties caused by adopting different theoretical color-temperature relations. We found that the Galactic bulge IMF can be fitted with two power laws with a break at M ∼0.56 M⊙, the slope being steeper (α = -2.41 ± 0.50) for the higher masses, and shallower (α = -1.25 ± 0.20) for the lower masses. In the high-mass range, our derived mass function agrees well with the mass function derived for other regions of the bulge. In the low-mass range however, our mass function is slightly shallower, which suggests that separating the disk and bulge components is particularly important in the low-mass range. The slope of the bulge mass function is also similar to the slope of the mass function derived for the disk in the high-mass regime, but the bulge mass function is slightly steeper in the low-mass regime. We used our new mass function to derive stellar mass-to-light values for the Galactic bulge and we obtained 2.1 < M/ LF814W < 2.4 and 3.1 < M/LF606W < 3.6 according to different assumptions on the slope of the IMF for masses larger than 1M⊙.

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Calamida A, Sahu KC, Casertano S, Anderson J, Cassisi S, Gennaro M et al. NEW INSIGHTS ON THE GALACTIC BULGE INITIAL MASS FUNCTION. Astrophysical Journal. 2015 Sep 1;810(1). 8. https://doi.org/10.1088/0004-637X/810/1/8