gjdonatiello
Phoenix Dwarf (ESO 245-7)
Phoenix Dwarf (ESO 245-7)
Credit: DESI LIS (DES1/DECaLS DR9, DR10), Giuseppe Donatiello
(RA/DEC: 27.7796, -44.4460 deg)
Initially believed by the discoverers to be a distant globular cluster [H.E. Schuster & R.M. West, A&A, Vol. 49, p. 129-131 (1976)], was later ascertained to be an irregular dwarf galaxy (dIrr) 440 ± 20 kpc (1.44 M light-years) distant.
Phoenix exhibits two distinct stellar populations. The older one is more present in the peripheral areas in a north-south direction, while the younger one dominates the central region, in particular in an east-west oriented bar structure. The rate of star formation appears to have been somewhat constant over time. These results, together with the morphological study, suggest the existence of an old population poor in metals with spheroidal symmetry around a younger internal component [D. Martinez-Delgado et al. (1999)].
New edited on Dec. 25, 2022
Acknowledgments
The Dark Energy Spectroscopic Instrument (DESI) data are licensed under the Creative Commons Attribution 4.0 International License (“CC BY 4.0”, Summary, Full Legal Code). Users are free to share, copy, redistribute, adapt, transform and build upon the DESI data available through this website for any purpose, including commercially.
This image used data obtained with the Dark Energy Spectroscopic Instrument (DESI). DESI construction and operations is managed by the Lawrence Berkeley National Laboratory. This material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of High-Energy Physics, under Contract No. DE–AC02–05CH11231, and by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract. Additional support for DESI was provided by the U.S. National Science Foundation (NSF), Division of Astronomical Sciences under Contract No. AST-0950945 to the NSF’s National Optical-Infrared Astronomy Research Laboratory; the Science and Technology Facilities Council of the United Kingdom; the Gordon and Betty Moore Foundation; the Heising-Simons Foundation; the French Alternative Energies and Atomic Energy Commission (CEA); the National Council of Science and Technology of Mexico (CONACYT); the Ministry of Science and Innovation of Spain (MICINN), and by the DESI Member Institutions: www.desi.lbl.gov/collaborating-institutions. The DESI collaboration is honored to be permitted to conduct scientific research on Iolkam Du’ag (Kitt Peak), a mountain with particular significance to the Tohono O’odham Nation. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the U.S. National Science Foundation, the U.S. Department of Energy, or any of the listed funding agencies.
Phoenix Dwarf (ESO 245-7)
Phoenix Dwarf (ESO 245-7)
Credit: DESI LIS (DES1/DECaLS DR9, DR10), Giuseppe Donatiello
(RA/DEC: 27.7796, -44.4460 deg)
Initially believed by the discoverers to be a distant globular cluster [H.E. Schuster & R.M. West, A&A, Vol. 49, p. 129-131 (1976)], was later ascertained to be an irregular dwarf galaxy (dIrr) 440 ± 20 kpc (1.44 M light-years) distant.
Phoenix exhibits two distinct stellar populations. The older one is more present in the peripheral areas in a north-south direction, while the younger one dominates the central region, in particular in an east-west oriented bar structure. The rate of star formation appears to have been somewhat constant over time. These results, together with the morphological study, suggest the existence of an old population poor in metals with spheroidal symmetry around a younger internal component [D. Martinez-Delgado et al. (1999)].
New edited on Dec. 25, 2022
Acknowledgments
The Dark Energy Spectroscopic Instrument (DESI) data are licensed under the Creative Commons Attribution 4.0 International License (“CC BY 4.0”, Summary, Full Legal Code). Users are free to share, copy, redistribute, adapt, transform and build upon the DESI data available through this website for any purpose, including commercially.
This image used data obtained with the Dark Energy Spectroscopic Instrument (DESI). DESI construction and operations is managed by the Lawrence Berkeley National Laboratory. This material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of High-Energy Physics, under Contract No. DE–AC02–05CH11231, and by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract. Additional support for DESI was provided by the U.S. National Science Foundation (NSF), Division of Astronomical Sciences under Contract No. AST-0950945 to the NSF’s National Optical-Infrared Astronomy Research Laboratory; the Science and Technology Facilities Council of the United Kingdom; the Gordon and Betty Moore Foundation; the Heising-Simons Foundation; the French Alternative Energies and Atomic Energy Commission (CEA); the National Council of Science and Technology of Mexico (CONACYT); the Ministry of Science and Innovation of Spain (MICINN), and by the DESI Member Institutions: www.desi.lbl.gov/collaborating-institutions. The DESI collaboration is honored to be permitted to conduct scientific research on Iolkam Du’ag (Kitt Peak), a mountain with particular significance to the Tohono O’odham Nation. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the U.S. National Science Foundation, the U.S. Department of Energy, or any of the listed funding agencies.