Leo P

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Leo P
Leo P color cutout hst 13376 08 acs wfc f814w f475w sci.jpg
Leo P by Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Leo
Right ascension 10h 21m 45.123s [1]
Declination +18° 05′ 16.89″ [1]
Distance 5,284 kly (1,620 kpc) [2]
Apparent magnitude  (V)16.89 [3]
Absolute magnitude  (V)−9.27 [2]
Characteristics
Type Irr
Size1132 pc [4] (3692.09 ly)
Apparent size  (V)1.2′ [2]
Other designations
Leo P, [1] AGC 208583

Leo P is a small, star-forming irregular galaxy located in the constellation Leo, discovered through the blind HI Arecibo Legacy Fast ALFA (ALFALFA) survey, as an ultra-compact high-velocity cloud (UCHVC) of hydrogen gas. Its confirmation as a dwarf galaxy in 2013 suggests that other such UCHVCs are possibly undiscovered dwarf galaxies themselves. [5] Leo P is noteworthy for harbouring one of the most metal-poor environments in the local universe. Its metallicity is just 3% that of the Sun's, meaning that its stars contain 30 times less heavy elements than the Sun. [2] This makes Leo P similar to the pristine environments of primordial galaxies.

Contents

Leo P is located on the very outskirts of the Local Group, nearly 5.3 million light years away, and may not be part of it, instead being part of the Antlia-Sextans Group, a small grouping of galaxies adjacent to the Local Group, sometimes considered bound to it.

Properties

Leo P is one of the smallest, least massive and faintest star-forming galaxies in the Local Group. Its total luminosity is less than 440,000 times that of the Sun (absolute magnitude of −9.27), and its stellar mass is only about 560,000 solar masses, implying a small stellar population. Leo P is also very rich in gas, containing about 810,000 solar masses of neutral hydrogen. [2] Leo P's half-light radius is about 570 pc. [4]

Leo P's stellar population consists of a strong concentration of massive, bright and blue stars in the centre of the galaxy, which may be B and A-type main sequence stars. Some fainter and redder stars are also observed, presumably red giants from an older stellar population. [3] 10 RR Lyrae stars have been detected in the galaxy, as well as one H II region, which is ionised by LP26, an O-type star of 22 solar masses, the only one in Leo P. [6]

Star formation

Leo P is one of the few Local Group galaxies which are currently forming stars. Its star formation rate is about 4.3×10−5  M☉ every year, [2] or 1 solar mass every 20,400 years, and it is the Local Group's most metal-poor star-forming galaxy. Its star formation history shows mostly constant star formation throughout its lifetime, something which is also observed in larger irregular galaxies. Models also suggest that there was not much star formation post-reionisation, 12–8 billion years ago, and over the last 4 billion years, star formation has been happening at a constant rate. [2]

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<span class="mw-page-title-main">Dwarf galaxy</span> Small galaxy composed of up to several billion stars

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Segue 1 is a dwarf spheroidal galaxy or globular cluster situated in the Leo constellation and discovered in 2006 by Sloan Digital Sky Survey. It is located at a distance of about 23 kpc from the Sun and moves away from the Sun with the velocity of about 206 km/s. Segue 1 has a noticeably elongated shape with the half-light radius of about 30 pc. This elongation may be caused by the tidal forces acting from the Milky Way galaxy if Segue 1 is being tidally disrupted now.

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<span class="mw-page-title-main">Hercules (dwarf galaxy)</span> Dwarf spheroidal galaxy in the constellation Hercules

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References

  1. 1 2 3 "Leo P". SIMBAD . Centre de données astronomiques de Strasbourg.
  2. 1 2 3 4 5 6 7 McQuinn, Kristen B. W.; Skillman, Evan D.; Dolphin, Andrew; Cannon, John M.; Salzer, John J.; Rhode, Katherine L.; Adams, Elizabeth A. K.; Berg, Danielle; Giovanelli, Riccardo; Girardi, Léo; Haynes, Martha P. (2015-10-01). "Leo P: An Unquenched Very Low-mass Galaxy". The Astrophysical Journal. 812 (2): 158. arXiv: 1506.05495 . Bibcode:2015ApJ...812..158M. doi: 10.1088/0004-637X/812/2/158 . ISSN   0004-637X.
  3. 1 2 Rhode, Katherine L.; Salzer, John J.; Haurberg, Nathalie C.; Van Sistine, Angela; Young, Michael D.; Haynes, Martha P.; Giovanelli, Riccardo; Cannon, John M.; Skillman, Evan D.; McQuinn, Kristen B. W.; Adams, Elizabeth A. K. (2013-06-01). "ALFALFA Discovery of the Nearby Gas-rich Dwarf Galaxy Leo P. II. Optical Imaging Observations". The Astronomical Journal. 145 (6): 149. arXiv: 1305.0270 . Bibcode:2013AJ....145..149R. doi: 10.1088/0004-6256/145/6/149 . ISSN   0004-6256.
  4. 1 2 Putman, Mary E.; Zheng, Yong; Price-Whelan, Adrian M.; Grcevich, Jana; Johnson, Amalya C.; Tollerud, Erik; Peek, Joshua E. G. (2021-05-01). "The Gas Content and Stripping of Local Group Dwarf Galaxies". The Astrophysical Journal. 913 (1): 53. arXiv: 2101.07809 . Bibcode:2021ApJ...913...53P. doi: 10.3847/1538-4357/abe391 . ISSN   0004-637X.
  5. ↑ Faerman, Yakov; Sternberg, Amiel; McKee, Christopher F. (2013-11-01). "Ultra-compact High Velocity Clouds as Minihalos and Dwarf Galaxies". The Astrophysical Journal. 777: 119. arXiv: 1309.0815 . doi:10.1088/0004-637X/777/2/119. ISSN   0004-637X.
  6. ↑ Telford, O. Grace; Chisholm, John; McQuinn, Kristen B. W.; Berg, Danielle A. (2021-12-01). "Far-ultraviolet Spectra of Main-sequence O Stars at Extremely Low Metallicity". The Astrophysical Journal. 922 (2): 191. arXiv: 2109.06885 . Bibcode:2021ApJ...922..191T. doi: 10.3847/1538-4357/ac1ce2 . ISSN   0004-637X.
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