The Dark Energy Spectroscopic Instrument (DESI)

Levi, Michael; Allen, Lori; Raichoor, Anand; Baltay, C.; BenZvi, S.; Beutler, Florian; Bolton, A.; Castander, F. J.; Chuang, Chia-Hsun; Cooper, Andrew P.; Cuby, Jean-Gabriel; Dey, Arjun; Eisenstein, Daniel; Fan, Xiaohui; Flaugher, B.; Frenk, Carlos S.; González‐Morales, Alma X.; Graur, Or; Guy, J.; Habib, Salman; Honscheid, K.; Juneau, Stéphanie; Kneib, Jean-Paul; Lahav, O.; Lang, Dustin; Leauthaud, Alexie; Lusso, Betta; Macorra, Axel de la; Manera, Marc; Martini, Paul; Mao, Shude; Newman, Jeffrey A.; Palanque-Delabrouille, N.; Percival, Will J.; Prieto, C. Allende; Rockosi, Constance M.; Ruhlmann-Kleider, V.; Schlegel, David J.; Seo, Hee-Jong; Song, Yong-Seon; Tarlè, G.; Weinberg, David H.; Yèche, Ch; Zu, Ying

doi:10.48550/arxiv.1907.10688

Cited by 51 publications

(62 citation statements)

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“…We plan to apply our methodology to mitigate the effects of strong molecular carbon veiling, which complicates identification of the continuum around the region of the Ca H & K lines and the CH G-band for other cool CEMP EMP/UMP candidates from: 1) our ongoing "Best and Farthest" survey (Yoon et al 2018a), observing with LBT/MODS and Gemini/GMOS, 2) numerous other cool CEMP stars with strong carbon veiling observed during the course of follow-up spectroscopy over the past few decades of metal-poor candidates from the HK survey (e.g., Beers et al 1992), 3) the list of CEMP candidates provided by Christlieb et al (2008), and 4) very cool CEMP stars from the medium-resolution spectroscopic surveys such as the SDSS, the AAOmega Evolution of Galactic Structure (AEGIS) survey (Yoon et al 2018b), and the Large Sky Area Multi-Object Fiber Spectroscopic Telescope survey (LAMOST; Cui et al 2012). This methodology can be widely applicable to numerous data from the future large moderate-resolution spectroscopic surveys such as the Dark Energy Spectroscopic Instrument(DESI; Levi et al 2019) survey, the William Herschel Telescope Enhanced Area Velocity Explorer (WEAVE; Dalton et al 2018) and 4MOST (de Jong et al 2019). These efforts will allow us not only to expedite the discovery process of the most metal-poor stars, but also to calculate frequencies of CEMP groups separately, and, in turn, provide insights regarding the shape of the FIMF.…”

Section: Discussionmentioning

confidence: 99%

Identification of a Group III CEMP-no Star in the Dwarf Spheroidal Galaxy Canes Venatici I

Yoon,

Whitten,

Beers

et al. 2019

Preprint

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CEMP-no stars, a subclass of carbon-enhanced metal-poor (CEMP) stars, are one of the most significant stellar populations in Galactic Archaeology, because they dominate the low end of the metallicity distribution function, providing information on the early star-formation and chemical-evolution history of the Milky Way and its satellite galaxies. Here we present an analysis of medium-resolution (R ∼ 1, 800) optical spectroscopy for a CEMP giant, SDSS J132755.56+333521.7, observed with the Large Binocular Telescope (LBT), one of the brightest (g ∼ 20.5) members of the classical dwarf spheroidal galaxy, Canes Venatici I (CVn I). Many CEMP stars discovered to date have very cool effective temperatures (T eff < 4500 K), resulting in strong veiling by molecular carbon bands over their optical spectra at low/medium spectral resolution. We introduce a technique to mitigate the carbon-veiling problem to obtain reliable stellar parameters, and validate this method with the LBT medium-resolution optical spectra of the ultra metal-poor ([Fe/H] = −4.0) CEMP-no dwarf, G 77-61, and seven additional very cool CEMP stars, which have published high-resolution spectroscopic parameters. We apply this technique to the LBT spectrum of SDSS J132755.56+333521.7. We find that this star is well-described with parameters T eff = 4530 K, log g = 0.7, [Fe/H] = −3.38, and absolute carbon abundance A(C) = 7.23, indicating that it is likely the first Group III CEMP-no star identified in CVn I. The Group III identification of this star suggests that it is a member of the extremely metal-poor population in CVn I, which may have been accreted into its halo.

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Section: Discussionmentioning

confidence: 99%

Identification of a Group III CEMP-no Star in the Dwarf Spheroidal Galaxy Canes Venatici I

Yoon,

Whitten,

Beers

et al. 2019

Preprint

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“…We explore whether such distinctions are within the reach of next generation surveys of distance and structure growth. Such experiments being conceived include DESI2 [1], FOBOS [2], LSSTspec [3], Mauna Kea Spectroscopic Explorer [4], MegaMapper [5], SpecTel [6], not to mention those using not galaxies as tracers but intensity mapping, Lyman alpha forest, etc. (see, e.g., [7]).…”

Section: Introductionmentioning

confidence: 99%

The Rise of Dark Energy

Linder¹

2021

Preprint

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“…Particularly, it is unclear whether the cool clouds are governed by random, inflowing, or outflowing motion (Lan & Mo 2019). In this paper, we explore the kinematics of MgII absorbers around a large sample of luminous red galaxies (LRGs) observed by the Baryon Oscillation Spectroscopic Survey (BOSS; Dawson et al 2013) at 𝑧∼0.55, in ★ E-mail: yingzu@sjtu.edu.cn hopes of paving the path for a self-consistent redshift-space distortion (RSD) modelling of metal absorbers with upcoming spectroscopic surveys like the DESI (Levi et al 2019) and PFS (Takada et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Kinematics of MgII Absorbers from the Redshift-space Distortion Around Massive Quiescent Galaxies

2021

Preprint

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The kinematics of MgII absorbers is the key to understanding the origin of cool, metalenriched gas clouds in the circumgalactic medium of massive quiescent galaxies. Exploiting the fact that the cloud line-of-sight velocity distribution is the only unknown for predicting the redshift-space distortion (RSD) of MgII absorbers from their 3D real-space distribution around galaxies, we develop a novel method to infer the cool cloud kinematics from the redshift-space galaxy-cloud cross-correlation 𝜉 𝑠 . We measure 𝜉 𝑠 for ∼10 4 MgII absorbers around ∼8×10 5 CMASS galaxies at 0.4<𝑧<0.8. We discover that 𝜉 𝑠 does not exhibit a strong Fingers-of-God effect, but is heavily truncated at velocity ∼300 km 𝑠 −1 . We reconstruct both the redshift and real-space cloud number density distributions inside haloes, 𝜉 𝑠 1ℎ and 𝜉 1ℎ , respectively. Thus, for any model of cloud kinematics, we can predict 𝜉 𝑠 1ℎ from the reconstructed 𝜉 1ℎ , and self-consistently compare to the observed 𝜉 𝑠 1ℎ . We consider four types of cloud kinematics, including an isothermal model with a single velocity dispersion, a satellite infall model in which cool clouds reside in the subhaloes, a cloud accretion model in which clouds follow the cosmic gas accretion, and a tired wind model in which clouds originate from the galactic wind-driven bubbles. All the four models provide statistically good fits to the RSD data, but only the tired wind model can reproduce the observed truncation by propagating ancient wind bubbles at ∼250 km 𝑠 −1 on scales ∼400 ℎ −1 kpc. Our method provides an exciting path to decoding the dynamical origin of metal absorbers from the RSD measurements with upcoming spectroscopic surveys.

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The Dark Energy Spectroscopic Instrument (DESI)

Cited by 51 publications

References 0 publications

Identification of a Group III CEMP-no Star in the Dwarf Spheroidal Galaxy Canes Venatici I

Identification of a Group III CEMP-no Star in the Dwarf Spheroidal Galaxy Canes Venatici I

The Rise of Dark Energy

Kinematics of MgII Absorbers from the Redshift-space Distortion Around Massive Quiescent Galaxies

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