SDSS-V Local Volume Mapper (LVM): A glimpse into Orion

K. Kreckel; O. V. Egorov; E. Egorova; G. A. Blanc; N. Drory; M. Kounkel; J. E. Méndez-Delgado; C. G. Román-Zúñiga; S. F. Sánchez; G. S. Stringfellow; A. M. Stutz; E. Zari; J. K. Barrera-Ballesteros; D. Bizyaev; J. R. Brownstein; E. Congiu; J. G. Fernández-Trincado; P. García; L. A. Hillenbrand; H. J. Ibarra-Medel; Y. Jin; E. J. Johnston; A. M. Jones; J. Serena Kim; J. A. Kollmeier; S. Kong; D. Krishnarao; N. Kumari; J. Li; K. S. Long; A. Mata-Sánchez; A. Mejía-Narváez; S. A. Popa; H. W. Rix; N. Sattler; J. Serna; A. Singh; J. R. Sánchez-Gallego; A. Wofford; T. Wong

doi:10.1051/0004-6361/202449943

SDSS-V Local Volume Mapper (LVM): A glimpse into Orion

K. Kreckel, O. V. Egorov, E. Egorova, G. A. Blanc, N. Drory, M. Kounkel, J. E. Méndez-Delgado, C. G. Román-Zúñiga, S. F. Sánchez, G. S. Stringfellow, A. M. Stutz, E. Zari, J. K. Barrera-Ballesteros, D. Bizyaev, J. R. Brownstein, E. Congiu, J. G. Fernández-Trincado, P. García, L. A. Hillenbrand, H. J. Ibarra-MedelY. Jin, E. J. Johnston, A. M. Jones, J. Serena Kim, J. A. Kollmeier, S. Kong, D. Krishnarao, N. Kumari, J. Li, K. S. Long, A. Mata-Sánchez, A. Mejía-Narváez, S. A. Popa, H. W. Rix, N. Sattler, J. Serna, A. Singh, J. R. Sánchez-Gallego, A. Wofford, T. Wong

Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

Context. The Orion Molecular Cloud complex, one of the nearest (D = 406 pc) and most extensively studied massive star-forming regions, is ideal for constraining the physics of stellar feedback, but its ∼12 deg diameter on the sky requires a dedicated approach to mapping ionized gas structures within and around the nebula. Aims. The Sloan Digital Sky Survey (SDSS-V) Local Volume Mapper (LVM) is a new optical integral field unit (IFU) that will map the ionized gas within the Milky Way and Local Group galaxies, covering 4300 deg² of the sky with the new LVM Instrument (LMV-I). Methods. We showcase optical emission line maps from LVM covering 12 deg² inside of the Orion belt region, with 195 000 individual spectra combined to produce images at 0.07 pc (35.3″) resolution. This is the largest IFU map made (to date) of the Milky Way, and contains well-known nebulae (the Horsehead Nebula, Flame Nebula, IC 434, and IC 432), as well as ionized interfaces with the neighboring dense Orion B molecular cloud. Results. We resolve the ionization structure of each nebula, and map the increase in both the [S II]/Hα and [N II]/Hα line ratios at the outskirts of nebulae and along the ionization front with Orion B. [O III] line emission is only spatially resolved within the center of the Flame Nebula and IC 434, and our ∼0.1 pc scale line ratio diagrams show how variations in these diagnostics are lost as we move from the resolved to the integrated view of each nebula. We detect ionized gas emission associated with the dusty bow wave driven ahead of the star σ Orionis, where the stellar wind interacts with the ambient interstellar medium. The Horsehead Nebula is seen as a dark occlusion of the bright surrounding photo-disassociation region. This small glimpse into Orion only hints at the rich science that will be enabled by the LVM.

Original language	English (US)
Article number	A352
Journal	Astronomy and Astrophysics
Volume	689
DOIs	https://doi.org/10.1051/0004-6361/202449943
State	Published - Sep 1 2024

Keywords

HII regions
ISM: clouds
ISM: general
Local insterstellar matter

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1051/0004-6361/202449943License: CC BY

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Kreckel, K., Egorov, O. V., Egorova, E., Blanc, G. A., Drory, N., Kounkel, M., Méndez-Delgado, J. E., Román-Zúñiga, C. G., Sánchez, S. F., Stringfellow, G. S., Stutz, A. M., Zari, E., Barrera-Ballesteros, J. K., Bizyaev, D., Brownstein, J. R., Congiu, E., Fernández-Trincado, J. G., García, P., Hillenbrand, L. A., ... Wong, T. (2024). SDSS-V Local Volume Mapper (LVM): A glimpse into Orion. Astronomy and Astrophysics, 689, Article A352. https://doi.org/10.1051/0004-6361/202449943

Kreckel, K, Egorov, OV, Egorova, E, Blanc, GA, Drory, N, Kounkel, M, Méndez-Delgado, JE, Román-Zúñiga, CG, Sánchez, SF, Stringfellow, GS, Stutz, AM, Zari, E, Barrera-Ballesteros, JK, Bizyaev, D, Brownstein, JR, Congiu, E, Fernández-Trincado, JG, García, P, Hillenbrand, LA, Ibarra-Medel, HJ, Jin, Y, Johnston, EJ, Jones, AM, Kim, JS, Kollmeier, JA, Kong, S, Krishnarao, D, Kumari, N, Li, J, Long, KS, Mata-Sánchez, A, Mejía-Narváez, A, Popa, SA, Rix, HW, Sattler, N, Serna, J, Singh, A, Sánchez-Gallego, JR, Wofford, A & Wong, T 2024, 'SDSS-V Local Volume Mapper (LVM): A glimpse into Orion', Astronomy and Astrophysics, vol. 689, A352. https://doi.org/10.1051/0004-6361/202449943

@article{0f560b7d0d9c48938f943115f0683eff,

title = "SDSS-V Local Volume Mapper (LVM): A glimpse into Orion",

abstract = "Context. The Orion Molecular Cloud complex, one of the nearest (D = 406 pc) and most extensively studied massive star-forming regions, is ideal for constraining the physics of stellar feedback, but its ∼12 deg diameter on the sky requires a dedicated approach to mapping ionized gas structures within and around the nebula. Aims. The Sloan Digital Sky Survey (SDSS-V) Local Volume Mapper (LVM) is a new optical integral field unit (IFU) that will map the ionized gas within the Milky Way and Local Group galaxies, covering 4300 deg2 of the sky with the new LVM Instrument (LMV-I). Methods. We showcase optical emission line maps from LVM covering 12 deg2 inside of the Orion belt region, with 195 000 individual spectra combined to produce images at 0.07 pc (35.3″) resolution. This is the largest IFU map made (to date) of the Milky Way, and contains well-known nebulae (the Horsehead Nebula, Flame Nebula, IC 434, and IC 432), as well as ionized interfaces with the neighboring dense Orion B molecular cloud. Results. We resolve the ionization structure of each nebula, and map the increase in both the [S II]/Hα and [N II]/Hα line ratios at the outskirts of nebulae and along the ionization front with Orion B. [O III] line emission is only spatially resolved within the center of the Flame Nebula and IC 434, and our ∼0.1 pc scale line ratio diagrams show how variations in these diagnostics are lost as we move from the resolved to the integrated view of each nebula. We detect ionized gas emission associated with the dusty bow wave driven ahead of the star σ Orionis, where the stellar wind interacts with the ambient interstellar medium. The Horsehead Nebula is seen as a dark occlusion of the bright surrounding photo-disassociation region. This small glimpse into Orion only hints at the rich science that will be enabled by the LVM.",

keywords = "HII regions, ISM: clouds, ISM: general, Local insterstellar matter",

author = "K. Kreckel and Egorov, {O. V.} and E. Egorova and Blanc, {G. A.} and N. Drory and M. Kounkel and M{\'e}ndez-Delgado, {J. E.} and Rom{\'a}n-Z{\'u}{\~n}iga, {C. G.} and S{\'a}nchez, {S. F.} and Stringfellow, {G. S.} and Stutz, {A. M.} and E. Zari and Barrera-Ballesteros, {J. K.} and D. Bizyaev and Brownstein, {J. R.} and E. Congiu and Fern{\'a}ndez-Trincado, {J. G.} and P. Garc{\'i}a and Hillenbrand, {L. A.} and Ibarra-Medel, {H. J.} and Y. Jin and Johnston, {E. J.} and Jones, {A. M.} and Kim, {J. Serena} and Kollmeier, {J. A.} and S. Kong and D. Krishnarao and N. Kumari and J. Li and Long, {K. S.} and A. Mata-S{\'a}nchez and A. Mej{\'i}a-Narv{\'a}ez and Popa, {S. A.} and Rix, {H. W.} and N. Sattler and J. Serna and A. Singh and S{\'a}nchez-Gallego, {J. R.} and A. Wofford and T. Wong",

note = "We thank the referee for their careful reading of this work and thoughtful suggestions. Funding for the Sloan Digital Sky Survey V has been provided by the Alfred P. Sloan Foundation, the Heising-Simons Foundation, the National Science Foundation, and the Participating Institutions. SDSS acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. SDSS telescopes are located at Apache Point Observatory, funded by the Astrophysical Research Consortium and operated by New Mexico State University, and at Las Campanas Observatory, operated by the Carnegie Institution for Science. The SDSS web site is www.sdss.org. SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration, including Caltech, The Carnegie Institution for Science, Chilean National Time Allocation Committee (CNTAC) ratified researchers, The Flatiron Institute, the Gotham Participation Group, Harvard University, Heidelberg University, The Johns Hopkins University, L'Ecole polytechnique f\u00E9d\u00E9rale de Lausanne (EPFL), Leibniz-Institut f\u00FCr Astrophysik Potsdam (AIP), Max-Planck-Institut f\u00FCr Astronomie (MPIA Heidelberg), MaxPlanck-Institut f\u00FCr Extraterrestrische Physik (MPE), Nanjing University, National Astronomical Observatories of China (NAOC), New Mexico State University, The Ohio State University, Pennsylvania State University, Smithsonian Astrophysical Observatory, Space Telescope Science Institute (STScI), the Stellar Astrophysics Participation Group, Universidad Nacional Aut\u00F3noma de M\u00E9xico, University of Arizona, University of Colorado Boulder, University of Illinois at Urbana-Champaign, University of Toronto, University of Utah, University of Virginia, Yale University, and Yunnan University. K.K., O.E., E.E., J.E.M.D., J.L., and N.S. gratefully acknowledge funding from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) in the form of an Emmy Noether Research Group (grant number KR4598/2-1, PI: Kreckel) and the European Research Council's starting grant ERC StG-101077573 (\{"}ISMMETALS\{"}). J.G.F-T gratefully acknowledges the grants support provided by Proyecto Fondecyt Iniciaci\u00F3n No. 11220340, Proyecto Fondecyt Postdoc No. 3230001 (Sponsoring researcher), from the Joint Committee ESO-Government of Chile under the agreement 2021 ORP 023/2021 and 2023 ORP 062/2023. C.R-Z. acknowledges support from project UNAM-PAPIIT IG101723 G.A.B. acknowledges the support from the ANID Basal project FB210003. AS gratefully acknowledges support by the Fondecyt Regular (project code 1220610), and ANID BASAL project FB210003. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France (Wenger et al. 2000). Multicolor images generated using the PYTHON package MULTICOLORFITS (Cigan 2019). This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Based in part on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. We thank the referee for their careful reading of this work and thoughtful suggestions. Funding for the Sloan Digital Sky Survey V has been provided by the Alfred P. Sloan Foundation, the Heising-Simons Foundation, the National Science Foundation, and the Participating Institutions. SDSS acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. SDSS telescopes are located at Apache Point Observatory, funded by the Astrophysical Research Consortium and operated by New Mexico State University, and at Las Campanas Observatory, operated by the Carnegie Institution for Science. The SDSS web site is www.sdss.org . SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration, including Caltech, The Carnegie Institution for Science, Chilean National Time Allocation Committee (CNTAC) ratified researchers, The Flatiron Institute, the Gotham Participation Group, Harvard University, Heidelberg University, The Johns Hopkins University, L\u2019Ecole polytechnique f\u00E9d\u00E9rale de Lausanne (EPFL), Leibniz-Institut f\u00FCr Astrophysik Potsdam (AIP), Max-Planck-Institut f\u00FCr Astronomie (MPIA Heidelberg), Max-Planck-Institut f\u00FCr Extraterrestrische Physik (MPE), Nanjing University, National Astronomical Observatories of China (NAOC), New Mexico State University, The Ohio State University, Pennsylvania State University, Smithsonian Astrophysical Observatory, Space Telescope Science Institute (STScI), the Stellar Astrophysics Participation Group, Universidad Nacional Aut\u00F3noma de M\u00E9xico, University of Arizona, University of Colorado Boulder, University of Illinois at Urbana-Champaign, University of Toronto, University of Utah, University of Virginia, Yale University, and Yunnan University. K.K., O.E., E.E., J.E.M.D., J.L., and N.S. gratefully acknowledge funding from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) in the form of an Emmy Noether Research Group (grant number KR4598/2-1, PI: Kreckel) and the European Research Council\u2019s starting grant ERC StG-101077573 (\u201CISM-METALS\u201D). J.G.F-T gratefully acknowledges the grants support provided by Proyecto Fondecyt Iniciaci\u00F3n No. 11220340, Proyecto Fondecyt Postdoc No. 3230001 (Sponsoring researcher), from the Joint Committee ESO-Government of Chile under the agreement 2021 ORP 023/2021 and 2023 ORP 062/2023. C.R-Z. acknowledges support from project UNAM-PAPIIT IG101723 G.A.B. acknowledges the support from the ANID Basal project FB210003. AS gratefully acknowledges support by the Fondecyt Regular (project code 1220610), and ANID BASAL project FB210003. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France (Wenger et al. 2000). Multicolor images generated using the PYTHON package MULTICOLORFITS (Cigan 2019). This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Based in part on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions.",

year = "2024",

month = sep,

day = "1",

doi = "10.1051/0004-6361/202449943",

language = "English (US)",

volume = "689",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

TY - JOUR

T1 - SDSS-V Local Volume Mapper (LVM)

T2 - A glimpse into Orion

AU - Kreckel, K.

AU - Egorov, O. V.

AU - Egorova, E.

AU - Blanc, G. A.

AU - Drory, N.

AU - Kounkel, M.

AU - Méndez-Delgado, J. E.

AU - Román-Zúñiga, C. G.

AU - Sánchez, S. F.

AU - Stringfellow, G. S.

AU - Stutz, A. M.

AU - Zari, E.

AU - Barrera-Ballesteros, J. K.

AU - Bizyaev, D.

AU - Brownstein, J. R.

AU - Congiu, E.

AU - Fernández-Trincado, J. G.

AU - García, P.

AU - Hillenbrand, L. A.

AU - Ibarra-Medel, H. J.

AU - Jin, Y.

AU - Johnston, E. J.

AU - Jones, A. M.

AU - Kim, J. Serena

AU - Kollmeier, J. A.

AU - Kong, S.

AU - Krishnarao, D.

AU - Kumari, N.

AU - Li, J.

AU - Long, K. S.

AU - Mata-Sánchez, A.

AU - Mejía-Narváez, A.

AU - Popa, S. A.

AU - Rix, H. W.

AU - Sattler, N.

AU - Serna, J.

AU - Singh, A.

AU - Sánchez-Gallego, J. R.

AU - Wofford, A.

AU - Wong, T.

N1 - We thank the referee for their careful reading of this work and thoughtful suggestions. Funding for the Sloan Digital Sky Survey V has been provided by the Alfred P. Sloan Foundation, the Heising-Simons Foundation, the National Science Foundation, and the Participating Institutions. SDSS acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. SDSS telescopes are located at Apache Point Observatory, funded by the Astrophysical Research Consortium and operated by New Mexico State University, and at Las Campanas Observatory, operated by the Carnegie Institution for Science. The SDSS web site is www.sdss.org. SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration, including Caltech, The Carnegie Institution for Science, Chilean National Time Allocation Committee (CNTAC) ratified researchers, The Flatiron Institute, the Gotham Participation Group, Harvard University, Heidelberg University, The Johns Hopkins University, L'Ecole polytechnique f\u00E9d\u00E9rale de Lausanne (EPFL), Leibniz-Institut f\u00FCr Astrophysik Potsdam (AIP), Max-Planck-Institut f\u00FCr Astronomie (MPIA Heidelberg), MaxPlanck-Institut f\u00FCr Extraterrestrische Physik (MPE), Nanjing University, National Astronomical Observatories of China (NAOC), New Mexico State University, The Ohio State University, Pennsylvania State University, Smithsonian Astrophysical Observatory, Space Telescope Science Institute (STScI), the Stellar Astrophysics Participation Group, Universidad Nacional Aut\u00F3noma de M\u00E9xico, University of Arizona, University of Colorado Boulder, University of Illinois at Urbana-Champaign, University of Toronto, University of Utah, University of Virginia, Yale University, and Yunnan University. K.K., O.E., E.E., J.E.M.D., J.L., and N.S. gratefully acknowledge funding from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) in the form of an Emmy Noether Research Group (grant number KR4598/2-1, PI: Kreckel) and the European Research Council's starting grant ERC StG-101077573 (\"ISMMETALS\"). J.G.F-T gratefully acknowledges the grants support provided by Proyecto Fondecyt Iniciaci\u00F3n No. 11220340, Proyecto Fondecyt Postdoc No. 3230001 (Sponsoring researcher), from the Joint Committee ESO-Government of Chile under the agreement 2021 ORP 023/2021 and 2023 ORP 062/2023. C.R-Z. acknowledges support from project UNAM-PAPIIT IG101723 G.A.B. acknowledges the support from the ANID Basal project FB210003. AS gratefully acknowledges support by the Fondecyt Regular (project code 1220610), and ANID BASAL project FB210003. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France (Wenger et al. 2000). Multicolor images generated using the PYTHON package MULTICOLORFITS (Cigan 2019). This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Based in part on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. We thank the referee for their careful reading of this work and thoughtful suggestions. Funding for the Sloan Digital Sky Survey V has been provided by the Alfred P. Sloan Foundation, the Heising-Simons Foundation, the National Science Foundation, and the Participating Institutions. SDSS acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. SDSS telescopes are located at Apache Point Observatory, funded by the Astrophysical Research Consortium and operated by New Mexico State University, and at Las Campanas Observatory, operated by the Carnegie Institution for Science. The SDSS web site is www.sdss.org . SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration, including Caltech, The Carnegie Institution for Science, Chilean National Time Allocation Committee (CNTAC) ratified researchers, The Flatiron Institute, the Gotham Participation Group, Harvard University, Heidelberg University, The Johns Hopkins University, L\u2019Ecole polytechnique f\u00E9d\u00E9rale de Lausanne (EPFL), Leibniz-Institut f\u00FCr Astrophysik Potsdam (AIP), Max-Planck-Institut f\u00FCr Astronomie (MPIA Heidelberg), Max-Planck-Institut f\u00FCr Extraterrestrische Physik (MPE), Nanjing University, National Astronomical Observatories of China (NAOC), New Mexico State University, The Ohio State University, Pennsylvania State University, Smithsonian Astrophysical Observatory, Space Telescope Science Institute (STScI), the Stellar Astrophysics Participation Group, Universidad Nacional Aut\u00F3noma de M\u00E9xico, University of Arizona, University of Colorado Boulder, University of Illinois at Urbana-Champaign, University of Toronto, University of Utah, University of Virginia, Yale University, and Yunnan University. K.K., O.E., E.E., J.E.M.D., J.L., and N.S. gratefully acknowledge funding from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) in the form of an Emmy Noether Research Group (grant number KR4598/2-1, PI: Kreckel) and the European Research Council\u2019s starting grant ERC StG-101077573 (\u201CISM-METALS\u201D). J.G.F-T gratefully acknowledges the grants support provided by Proyecto Fondecyt Iniciaci\u00F3n No. 11220340, Proyecto Fondecyt Postdoc No. 3230001 (Sponsoring researcher), from the Joint Committee ESO-Government of Chile under the agreement 2021 ORP 023/2021 and 2023 ORP 062/2023. C.R-Z. acknowledges support from project UNAM-PAPIIT IG101723 G.A.B. acknowledges the support from the ANID Basal project FB210003. AS gratefully acknowledges support by the Fondecyt Regular (project code 1220610), and ANID BASAL project FB210003. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France (Wenger et al. 2000). Multicolor images generated using the PYTHON package MULTICOLORFITS (Cigan 2019). This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Based in part on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions.

PY - 2024/9/1

Y1 - 2024/9/1

N2 - Context. The Orion Molecular Cloud complex, one of the nearest (D = 406 pc) and most extensively studied massive star-forming regions, is ideal for constraining the physics of stellar feedback, but its ∼12 deg diameter on the sky requires a dedicated approach to mapping ionized gas structures within and around the nebula. Aims. The Sloan Digital Sky Survey (SDSS-V) Local Volume Mapper (LVM) is a new optical integral field unit (IFU) that will map the ionized gas within the Milky Way and Local Group galaxies, covering 4300 deg2 of the sky with the new LVM Instrument (LMV-I). Methods. We showcase optical emission line maps from LVM covering 12 deg2 inside of the Orion belt region, with 195 000 individual spectra combined to produce images at 0.07 pc (35.3″) resolution. This is the largest IFU map made (to date) of the Milky Way, and contains well-known nebulae (the Horsehead Nebula, Flame Nebula, IC 434, and IC 432), as well as ionized interfaces with the neighboring dense Orion B molecular cloud. Results. We resolve the ionization structure of each nebula, and map the increase in both the [S II]/Hα and [N II]/Hα line ratios at the outskirts of nebulae and along the ionization front with Orion B. [O III] line emission is only spatially resolved within the center of the Flame Nebula and IC 434, and our ∼0.1 pc scale line ratio diagrams show how variations in these diagnostics are lost as we move from the resolved to the integrated view of each nebula. We detect ionized gas emission associated with the dusty bow wave driven ahead of the star σ Orionis, where the stellar wind interacts with the ambient interstellar medium. The Horsehead Nebula is seen as a dark occlusion of the bright surrounding photo-disassociation region. This small glimpse into Orion only hints at the rich science that will be enabled by the LVM.

AB - Context. The Orion Molecular Cloud complex, one of the nearest (D = 406 pc) and most extensively studied massive star-forming regions, is ideal for constraining the physics of stellar feedback, but its ∼12 deg diameter on the sky requires a dedicated approach to mapping ionized gas structures within and around the nebula. Aims. The Sloan Digital Sky Survey (SDSS-V) Local Volume Mapper (LVM) is a new optical integral field unit (IFU) that will map the ionized gas within the Milky Way and Local Group galaxies, covering 4300 deg2 of the sky with the new LVM Instrument (LMV-I). Methods. We showcase optical emission line maps from LVM covering 12 deg2 inside of the Orion belt region, with 195 000 individual spectra combined to produce images at 0.07 pc (35.3″) resolution. This is the largest IFU map made (to date) of the Milky Way, and contains well-known nebulae (the Horsehead Nebula, Flame Nebula, IC 434, and IC 432), as well as ionized interfaces with the neighboring dense Orion B molecular cloud. Results. We resolve the ionization structure of each nebula, and map the increase in both the [S II]/Hα and [N II]/Hα line ratios at the outskirts of nebulae and along the ionization front with Orion B. [O III] line emission is only spatially resolved within the center of the Flame Nebula and IC 434, and our ∼0.1 pc scale line ratio diagrams show how variations in these diagnostics are lost as we move from the resolved to the integrated view of each nebula. We detect ionized gas emission associated with the dusty bow wave driven ahead of the star σ Orionis, where the stellar wind interacts with the ambient interstellar medium. The Horsehead Nebula is seen as a dark occlusion of the bright surrounding photo-disassociation region. This small glimpse into Orion only hints at the rich science that will be enabled by the LVM.

KW - HII regions

KW - ISM: clouds

KW - ISM: general

KW - Local insterstellar matter

UR - http://www.scopus.com/inward/record.url?scp=85205375390&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85205375390&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202449943

DO - 10.1051/0004-6361/202449943

M3 - Article

AN - SCOPUS:85205375390

SN - 0004-6361

VL - 689

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A352

ER -

SDSS-V Local Volume Mapper (LVM): A glimpse into Orion

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