SDSS-V Local Volume Mapper (LVM): A glimpse into Orion
Kathryn Kreckel, Oleg V. Egorov, E. S. Egorova, Guillermo A. Blanc, Niv Drory, Marina Kounkel, J. Eduardo Méndez-Delgado, C. Román-Zúñiga, S. F. Sánchez, Guy S. Stringfellow, Amelia M. Stutz, Eleonora Zari, J. K. Barrera-Ballesteros, Dmitry Bizyaev, Joel R. Brownstein, Enrico Congiu, José G. Fernández-Trincado, P. García, Lynne A. Hillenbrand, Héctor J. Ibarra-Medel, Yu Jin, Evelyn J. Johnston, Amy Jones, Jinyoung Serena Kim, Juna A. Kollmeier, Shuo Kong, Dhanesh Krishnarao, Nimisha Kumari, J. Li, K. S. Long, A. Mata-Sánchez, A. Mejía-Narváez, S. A. Popa, Hans‐Walter Rix, Natascha Sattler, Javier Serna, Amrita Singh, José Sánchez-Gallego, Aida Wofford, Tony Wong
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 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 ]/Hα and [N II ]/H α 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.