From evolved stars to the evolution of IC 1613. (arXiv:1812.07230v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Hashemi_S/0/1/0/all/0/1">Seyed Azim Hashemi</a> (Sharif University, Iran), <a href="http://arxiv.org/find/astro-ph/1/au:+Javadi_A/0/1/0/all/0/1">Atefeh Javadi</a> (IPM, Iran), <a href="http://arxiv.org/find/astro-ph/1/au:+Loon_J/0/1/0/all/0/1">Jacco Th. van Loon</a> (Keele University, UK)
IC 1613 is a Local Group dwarf irregular galaxy at a distance of 750 kpc. In
this work, we present an analysis of the star formation history (SFH) of a
field of $sim200$ square arcmin in the central part of the galaxy. To this
aim, we use a novel method based on the resolved population of more highly
evolved stars. We identify 53 such stars, 8 of which are supergiants and the
remainder are long period variables (LPV), large amplitude variables (LAV) or
extreme Asymptotic Giant Branch (x-AGB) stars. Using stellar evolution models,
we find the age and birth mass of these stars and thus reconstruct the SFH. The
average rate of star formation during the last Gyr is $sim3times10^{-4}$
M$_odot$ yr$^{-1}$ kpc$^{-2}$. The absence of a dominant epoch of star
formation over the past 5 Gyr, suggests that IC 1613 has evolved in isolation
for that long, spared harrassment by other Local Group galaxies (in particular
M 31 and the Milky Way). We confirm the radial age gradient, with star
formation currently concentrated in the central regions of IC 1613, and the
failure of recent star formation to have created the main HI supershell. Based
on the current rate of star formation at $(5.5pm2)times10^{-3}$ M$_odot$
yr$^{-1}$, the interstellar gas mass of the galaxy of $9times10^7$ M$_odot$
and the gas production rate from AGB stars at $sim6times10^{-4}$ M$_odot$
yr$^{-1}$, we conclude that the star formation activity of IC 1613 can continue
for $sim18$ Gyr in a closed-box model, but is likely to cease much earlier
than that unless gas can be accreted from outside.
IC 1613 is a Local Group dwarf irregular galaxy at a distance of 750 kpc. In
this work, we present an analysis of the star formation history (SFH) of a
field of $sim200$ square arcmin in the central part of the galaxy. To this
aim, we use a novel method based on the resolved population of more highly
evolved stars. We identify 53 such stars, 8 of which are supergiants and the
remainder are long period variables (LPV), large amplitude variables (LAV) or
extreme Asymptotic Giant Branch (x-AGB) stars. Using stellar evolution models,
we find the age and birth mass of these stars and thus reconstruct the SFH. The
average rate of star formation during the last Gyr is $sim3times10^{-4}$
M$_odot$ yr$^{-1}$ kpc$^{-2}$. The absence of a dominant epoch of star
formation over the past 5 Gyr, suggests that IC 1613 has evolved in isolation
for that long, spared harrassment by other Local Group galaxies (in particular
M 31 and the Milky Way). We confirm the radial age gradient, with star
formation currently concentrated in the central regions of IC 1613, and the
failure of recent star formation to have created the main HI supershell. Based
on the current rate of star formation at $(5.5pm2)times10^{-3}$ M$_odot$
yr$^{-1}$, the interstellar gas mass of the galaxy of $9times10^7$ M$_odot$
and the gas production rate from AGB stars at $sim6times10^{-4}$ M$_odot$
yr$^{-1}$, we conclude that the star formation activity of IC 1613 can continue
for $sim18$ Gyr in a closed-box model, but is likely to cease much earlier
than that unless gas can be accreted from outside.
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