A Search for RR Lyrae Stars in Segue 2 and Segue 3
E Boettcher, B Willman, R Fadely… - The Astronomical …, 2013 - iopscience.iop.org
We present an extensive search for RR Lyrae (RRL) stars in and around the ultra-faint Milky
Way companions Segue 2 and Segue 3. The former (MV=− 2.5) appears to be an extremely
faint dwarf galaxy companion of the Milky Way. The latter (MV= 0.0) is among the faintest
star clusters known. We use B and V band time-series imaging obtained at the WIYN 0.9 m
telescope at Kitt Peak National Observatory to search for RRL in these objects. In our Segue
2 observations, we present a previously unknown fundamental mode (RRab) RRL star with …
Way companions Segue 2 and Segue 3. The former (MV=− 2.5) appears to be an extremely
faint dwarf galaxy companion of the Milky Way. The latter (MV= 0.0) is among the faintest
star clusters known. We use B and V band time-series imaging obtained at the WIYN 0.9 m
telescope at Kitt Peak National Observatory to search for RRL in these objects. In our Segue
2 observations, we present a previously unknown fundamental mode (RRab) RRL star with …
A Search for RR Lyrae Stars in Segue 2 and Segue 3
B Willman - 2013 - scholarship.haverford.edu
We present an extensive search for RR Lyrae (RRL) stars in and around the ultra-faint Milky
Way companions Segue 2 and Segue 3. The former (MV=–2.5) appears to be an extremely
faint dwarf galaxy companion of the Milky Way. The latter (MV= 0.0) is among the faintest
star clusters known. We use B and V band time-series imaging obtained at the WIYN 0.9 m
telescope at Kitt Peak National Observatory to search for RRL in these objects. In our Segue
2 observations, we present a previously unknown fundamental mode (RRab) RRL star with …
Way companions Segue 2 and Segue 3. The former (MV=–2.5) appears to be an extremely
faint dwarf galaxy companion of the Milky Way. The latter (MV= 0.0) is among the faintest
star clusters known. We use B and V band time-series imaging obtained at the WIYN 0.9 m
telescope at Kitt Peak National Observatory to search for RRL in these objects. In our Segue
2 observations, we present a previously unknown fundamental mode (RRab) RRL star with …
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