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

被引：5

作者：

Kreckel, K. ^{[1
]}

Egorov, O. V. ^{[1
]}

Egorova, E. ^{[1
]}

Blanc, G. A. ^{[2
,3
]}

Drory, N. ^{[4
]}

Kounkel, M. ^{[5
]}

Mendez-Delgado, J. E. ^{[1
]}

Roman-Zuniga, C. G. ^{[6
]}

Sanchez, S. F. ^{[6
]}

Stringfellow, G. S. ^{[7
]}

Stutz, A. M. ^{[8
,9
,10
]}

Zari, E. ^{[11
]}

Barrera-Ballesteros, J. K. ^{[6
]}

Bizyaev, D. ^{[12
,13
]}

Brownstein, J. R. ^{[14
]}

Congiu, E. ^{[15
]}

Fernandez-Trincado, J. G. ^{[17
]}

Garcia, P. ^{[16
,17
]}

Hillenbrand, L. A. ^{[18
]}

Ibarra-Medel, H. J. ^{[19
]}

Jin, Y. ^{[20
]}

Johnston, E. J. ^{[21
]}

Jones, A. M. ^{[22
]}

Kim, J. Serena ^{[23
]}

Kollmeier, J. A. ^{[2
,24
]}

Kong, S. ^{[23
]}

Krishnarao, D. ^{[25
]}

Kumari, N. ^{[22
]}

Li, J. ^{[1
]}

Long, K. S. ^{[22
]}

Mata-Sanchez, A. ^{[19
]}

Mejia-Narvaez, A. ^{[3
]}

Popa, S. A. ^{[1
]}

Rix, H. -W. ^{[11
]}

Sattler, N. ^{[1
]}

Serna, J. ^{[6
,26
]}

Singh, A. ^{[3
]}

Sanchez-Gallego, J. R. ^{[27
]}

Wofford, A. ^{[6
,28
]}

Wong, T. ^{[29
]}

机构：

[1] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany

[2] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA

[3] Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile

[4] Univ Texas Austin, McDonald Observ, 1 Univ Stn, Austin, TX 78712 USA

[5] Univ North Florida, Dept Phys, 1 UNF Dr, Jacksonville, FL 32224 USA

[6] Univ Nacl Autonoma Mexico, Inst Astron, AP 106, Ensenada 22800, BC, Mexico

[7] Univ Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA

[8] Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion, Chile

[9] CNRS, Franco Chilean Lab Astron, IRL 3386, Santiago, Chile

[10] Univ Chile, Santiago, Chile

[11] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[12] Apache Point Observ, POB 59, Sunspot, NM 88349 USA

[13] New Mexico State Univ, POB 59, Sunspot, NM 88349 USA

[14] Univ Utah, Dept Phys & Astron, 115 S 1400 E, Salt Lake City, UT 84112 USA

[15] European Southern Observ, Ave Alonso Cordoba 3107,Casilla 19, Santiago 19001, Chile

[16] Chinese Acad Sci, CAS, South Amer Ctr Astron, Natl Astron Observ, Beijing 100101, Peoples R China

[17] Univ Catolica Norte, Inst Astron, Av Angamos 0610, Antofagasta, Chile

[18] CALTECH, Dept Astron, Pasadena, CA 91125 USA

[19] Univ Nacl Autonoma Mexico, Inst Astron, AP 70-264, Mexico City 04510, Mexico

[20] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[21] Univ Diego Portales, Fac Ingn & Ciencias, Inst Estudios Astrofis, Av Ejercito Libertador 441, Santiago, Chile

[22] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[23] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA

[24] Univ Toronto, Canadian Inst Theoret Astrophys CITA, 60 St George St, Toronto, ON M5S 3H8, Canada

[25] Colorado Coll, Dept Phys, Colorado Springs, CO 80903 USA

[26] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA

[27] Univ Washington, Dept Astron, Seattle, WA 98195 USA

[28] Univ Calif San Diego, Ctr Astrophys & Space Sci, Dept Phys, 9500 Gilman Dr, La Jolla, CA 92093 USA

[29] Univ Illinois, Dept Astron, Urbana, IL 61801 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 689卷

基金：

欧洲研究理事会; 美国国家科学基金会; 美国国家航空航天局;

关键词：

ISM: clouds; ISM: general; HII regions; local insterstellar matter; SPACE-TELESCOPE SURVEY; WARM IONIZED MEDIUM; H-II REGIONS; PHYSICAL CONDITIONS; PHOTODISSOCIATION REGIONS; MASSIVE STARS; CHEMICAL-COMPOSITION; MOLECULAR CLOUD; APOGEE-2; SURVEY; BARNARDS LOOP;

D O I：

10.1051/0004-6361/202449943

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 similar to 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 deg(2) of the sky with the new LVM Instrument (LMV-I). Methods. We showcase optical emission line maps from LVM covering 12 deg(2) 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]/H alpha and [N II]/H alpha 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 similar to 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 sigma 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.

引用

页数：13

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