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Paper   IPM / Astronomy / 16581
School of Astronomy
  Title:   The Isaac Newton Telescope Monitoring Survey of Local Group Dwarf Galaxies. IV. The Star Formation History of Andromeda VII Derived from Long-period Variable Stars
  Author(s): 
1.  Mahdieh . Navabi
2.  Elham . Saremi
3.  Atefeh . Javadi
4.  Majedeh . Noori
5.  Jacco . Th. van Loon
6.  Habib . G. Khosroshahi
7.  Iain . McDonald
8.  Mina . Alizadeh
9.  Arash . Danesh
10.  Ghassem . Gozaliasl
11.  Alireza . Molaeinezhad
12.  Tahere . Parto
13.  Mojtaba . Raouf
  Status:   Published
  Journal: ApJ
  No.:  2
  Vol.:  910
  Year:  2021
  Supported by:            ipm IPM
  Abstract:
We have examined the star formation history (SFH) of Andromeda VII (And VII), the brightest and most massive dwarf spheroidal (dSph) satellite of the Andromeda galaxy (M31). Although M31 is surrounded by several dSph companions with old stellar populations and low metallicity, it has a metal-rich stellar halo with an age of 6–8 Gyr. This indicates that any evolutionary association between the stellar halo of M31 and its dSph system is frail. Therefore, the question is whether And VII (a high-metallicity dSph located  220 kpc from M31) can be associated with M31's young, metal-rich halo. Here we perform the first reconstruction of the SFH of And VII employing long-period variable (LPV) stars. As the most evolved asymptotic giant branch and red supergiant stars, the birth mass of LPVs can be determined by connecting their near-infrared photometry to theoretical evolutionary tracks. We found 55 LPV candidates within two half-light radii, using multiepoch imaging with the Isaac Newton Telescope in the i and V bands. Based on their birth mass function, the star formation rate (SFR) of And VII was obtained as a function of cosmic time. The main epoch of star formation occurred sime 6.2 Gyr ago with an SFR of 0.006 ± 0.002 M⊙ yr−1. Over the past 6 Gyr, we find slow star formation, which continued until 500 Myr ago with an SFR   0.0005 ± 0.0002 M yr−1. We determined And VII's stellar mass M = (13.3 ± 5.3) × 106 M within a half-light radius r\tfrac12=3. ′ 8±0. ′ 3 and metallicity Z = 0.0007, and we also derived its distance modulus of μ = 24.38 mag.

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