Stellar Properties for a Comprehensive Collection of Star-forming Regions in the SDSS APOGEE-2 Survey*

Román-Zúñiga, C.; Kounkel, Marina; Hernández, Jesús; Ramírez, K. Peña; López-Valdivia, Ricardo; Covey, Kevin R.; Stutz, Amelia M.; Roman-Lopes, Alexandre; Campbell, Hunter; Khilfeh, Elliott; Tapia, M.; Stringfellow, Guy S.; Downes, Juan José; Stassun, Keivan G.; Minniti, D.; Bayo, A.; Kim, Jinyoung Serena; Suárez, Genaro; Ybarra, Jason E.; Fernández-Trincado, J. G.; Longa-Peña, Penélope; Ramírez-Preciado, Valeria; Serna, Javier; García-Hernández, D. A.; Beaton, Rachael L.; Bizyaev, Dmitry; Pan, Kaike

doi:10.3847/1538-3881/aca3a4

Cited by 6 publications

(3 citation statements)

References 84 publications

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“…SDSS-IV expanded its footprint in the targeting of YSOs and complemented previous data by observing the Orion Complex (Cottle et al 2018), the Taurus Molecular Clouds, Upper Sco, W3/W4/W5 clusters, Cygnus X, Rosette Nebula, Carina Nebula, more evolved clusters such as the Pleiades and α Per, and others (for a complete overview of the regions observed, see Román-Zúñiga et al 2023). With respect to SDSS-III, a greater emphasis was given to targeting sources in a more homogeneous manner, for instance by using color cuts or photometric variability to select sources rather than relying on existing confirmation of their youth.…”

Section: Introductionmentioning

confidence: 87%

“…Most of these are evolved stars; in particular red giants have historically been favored for the observations due to the ability to use them as tracers of stellar populations at large distances. However, SDSS has observed spectra of thousands of young stellar objects (YSOs) through its auxiliary programs (Román-Zúñiga et al 2023).…”

Section: Introductionmentioning

confidence: 99%

“…With respect to SDSS-III, a greater emphasis was given to targeting sources in a more homogeneous manner, for instance by using color cuts or photometric variability to select sources rather than relying on existing confirmation of their youth. However different selection criteria were developed for each individual region, because the observations fell under the auspices of various programs (Beaton et al 2021;Santana et al 2021;Román-Zúñiga et al 2023). Spectra of >30,000 stars were taken across the plates covering these regions.…”

Section: Introductionmentioning

confidence: 99%

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ABYSS. I. Targeting Strategy for the APOGEE and BOSS Young Star Survey in SDSS-V

Kounkel

Zari

Covey

et al. 2023

ApJS

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The fifth iteration of the Sloan Digital Sky Survey is set to obtain optical and near-infrared spectra of ∼5 million stars of all ages and masses throughout the Milky Way. As a part of these efforts, APOGEE and BOSS Young Star Survey (ABYSS) will observe ∼105 stars with ages <30 Myr that have been selected using a set of homogeneous selection functions that make use of different tracers of youth. The ABYSS targeting strategy we describe in this paper is aimed to provide the largest spectroscopic census of young stars to date. It consists of eight different types of selection criteria that take the position on the H-R diagram, infrared excess, variability, as well as the position in phase space in consideration. The resulting catalog of ∼200,000 sources (of which a half are expected to be observed) provides representative coverage of the young Galaxy, including both nearby diffuse associations as well as more distant massive complexes, reaching toward the inner Galaxy and the Galactic center.

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Section: Introductionmentioning

confidence: 87%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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ABYSS. I. Targeting Strategy for the APOGEE and BOSS Young Star Survey in SDSS-V

Kounkel

Zari

Covey

et al. 2023

ApJS

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Spectroscopic substellar initial mass function of NGC 2244

Almendros-Abad¹,

Mužić²,

Bouy³

et al. 2023

A&A

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Context. The dominant formation channel of brown dwarfs (BDs) is not well constrained yet and a promising way to discriminate between scenarios is to test the environment-dependent efficiency in forming BDs. So far, the outcome of star formation, studied through the initial mass function, has been found to be very similar in all clusters that have been inspected. Aims. We aim to characterize the low-mass (sub)stellar population of the central portion (2.4 pc2) of the ∼2 Myr old cluster NGC 2244 using near-infrared spectroscopy. By studying this cluster, characterized by a low stellar density and numerous OB stars, we aim to explore the effect that OB stars may have on the production of BDs. Methods. We obtained near-infrared HK spectroscopy of 85 faint candidate members of NGC 2244. We derived the spectral type and extinction by comparison with spectral templates. We evaluated cluster membership using three gravity-sensitive spectral indices based on the shape of the H-band. Furthermore, we evaluated the infrared excess from Spitzer of all the candidate members of the cluster. Finally, we estimated the mass of all the candidate members of the cluster and derived the initial mass function, star-to-BD number ratio, and disk fraction. Results. The initial mass function is well represented by a power law (dN/dM ∝ M−α) below 0.4 M⊙, with a slope α = 0.7–1.1 depending on the fitted mass range. We calculated a star-to-BD number ratio of 2.2–2.8. We find the low-mass population of NGC 2244 to be consistent with nearby star-forming regions, although it is at the high end of BD production. We find BDs in NGC 2244 to be, on average, closer to OB stars than to low-mass stars, which could potentially be the first piece of evidence that OB stars affect the formation of BDs. We find a disk fraction of all the members with a spectral type later than K0 of 39 ± 9% which is lower than typical values found in nearby star-forming regions of similar ages.

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

Kreckel,

Egorov,

Egorova

et al. 2024

A&A

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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 sim 12 deg diameter on the sky requires a dedicated approach to mapping ionized gas structures within and around the nebula. 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). 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. We resolve the ionization structure of each nebula, and map the increase in both the and line ratios at the outskirts of nebulae and along the ionization front with Orion B. line emission is only spatially resolved within the center of the Flame Nebula and IC 434, and our sim 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.

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Stellar Properties for a Comprehensive Collection of Star-forming Regions in the SDSS APOGEE-2 Survey*

Cited by 6 publications

References 84 publications

ABYSS. I. Targeting Strategy for the APOGEE and BOSS Young Star Survey in SDSS-V

ABYSS. I. Targeting Strategy for the APOGEE and BOSS Young Star Survey in SDSS-V

Spectroscopic substellar initial mass function of NGC 2244

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

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