Tucana B: An Isolated and Quenched Ultra-faint Dwarf Galaxy at D=1.4 Mpc

Sand, D. J.; Mutlu-Pakdil, B.; Jones, M. G.; Karunakaran, A.; Wang, F.; Yang, J.; Chiti, A.; Bennet, P.; Crnojević, D.; Spekkens, K.

doi:10.48550/arxiv.2205.09129

Cited by 6 publications

(7 citation statements)

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“…There are about 60 known satellite galaxies of the MW [438], many of which have measurements of stellar kinematics from large ground-based telescopes and orbital properties (such as pericenter distances) constrained with Gaia data. Several surveys are now able to detect satellites in MW-like galaxies in the Local Volume and this number will grow in the coming years [439,437,440,441,56,442,443,444,445,446,447,448,449,450]. The implications of these measurements for general SIDM models remains to be fully explored.…”

Section: Dwarf Galaxies In the Local Group And Beyondmentioning

confidence: 99%

Astrophysical Tests of Dark Matter Self-Interactions

Adhikari¹,

Banerjee²,

Boddy³

et al. 2022

Preprint

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Self-interacting dark matter (SIDM) arises generically in scenarios for physics beyond the Standard Model that have dark sectors with light mediators or strong dynamics. The selfinteractions allow energy and momentum transport through halos, altering their structure and dynamics relative to those produced by collisionless dark matter. SIDM models provide a promising way to explain the diversity of galactic rotation curves, and they form a predictive and versatile framework for interpreting astrophysical phenomena related to dark matter.This review provides a comprehensive explanation of the physical effects of dark matter self-interactions in objects ranging from galactic satellites (dark and luminous) to clusters of galaxies and the large-scale structure. The second major part describes the methods used to constrain SIDM models including current constraints, with the aim of advancing tests with upcoming galaxy surveys. This part also provides a detailed review of the unresolved small-scale structure formation issues and concrete ways to test simple SIDM models. The

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Section: Dwarf Galaxies In the Local Group And Beyondmentioning

confidence: 99%

Astrophysical Tests of Dark Matter Self-Interactions

Adhikari¹,

Banerjee²,

Boddy³

et al. 2022

Preprint

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“…The discovery and study of dwarf galaxies in the Local Group has prospered due to the great advances in wide field imaging surveys over the last two decades (e.g. Willman et al 2005a,b;Belokurov et al 2006Belokurov et al , 2007Belokurov et al , 2008Laevens et al 2015a,b;Koposov et al 2015a;Torrealba et al 2016Torrealba et al , 2018Torrealba et al , 2019Mau et al 2020;Cerny et al 2021aCerny et al ,b, 2022Sand et al 2022). The Sloan Digital Sky Survey (SDSS; York et al 2000;Abazajian et al 2009) led the early charge, with the Pan-STARRS consortium (Chambers et al 2016), the Dark Energy Survey (DES; Abbott et al 2018), and the DECam Local Volume Exploration Survey (DELVE; Drlica-Wagner et al 2021) contributing mightily to the discovery of Milky Way satellites, while the Pan-Andromeda Archaeological Survey (PAndAS; McConnachie et al 2009) has been prolific in finding dwarf galaxies around M31 (e.g.…”

Section: Introductionmentioning

confidence: 99%

Discovery of a new Local Group Dwarf Galaxy Candidate in UNIONS: Boötes V

T.¹,

Jensen²,

Roediger³

et al. 2022

Preprint

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We present the discovery of Boötes V, a new ultra-faint dwarf galaxy candidate. This satellite is detected as a resolved overdensity of stars during an ongoing search for new Local Group dwarf galaxy candidates in the UNIONS photometric dataset. It has a physical half-light radius of 26.9 +7.5 −5.4 pc, a V -band magnitude of −4.5 ± 0.4 mag, and resides at a heliocentric distance of approximately 100 kpc. We use Gaia DR3 astrometry to identify member stars, characterize the systemic proper motion, and confirm the reality of this faint stellar system. The brightest star in this system was followed up using Gemini GMOS-N long-slit spectroscopy and is measured to have a metallicity of [Fe/H] = -2.85 ± 0.10 dex and a heliocentric radial velocity of v r = 5.1 ± 13.4 km s −1 . Boötes V is larger (in terms of scale radius), more distant, and more metal-poor than the vast majority of globular clusters. It is likely that Boötes V is an ultra-faint dwarf galaxy, though future spectroscopic studies will be necessary to definitively classify this object.

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“…All three show little to no gas content and predominantly old stellar populations formed roughly ∼ 9-10 Gyrs ago (Castellani et al 1996;Monelli et al 2010a,b;Savino et al 2019;Makarova et al 2017). Further away, at ∼ 2 Mpc, the only other examples of quiescent dwarfs known are KKR25 and KKs3 (Karachentsev et al 2015(Karachentsev et al , 2001, plus the recent discoveries of Tucana B (Sand et al 2022) and COSMOS-dw1 in the COSMOS-CANDELS field beyond the LG (Polzin et al 2021).…”

Section: Introductionmentioning

confidence: 99%

The Tucana dwarf spheroidal: a distant backsplash galaxy of M31?

Santos-Santos¹,

Navarro²,

McConnachie³

2022

Preprint

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We use the APOSTLE suite of Local Group (LG) cosmological hydrodynamical simulations to examine the properties of "backsplash" galaxies, i.e, dwarfs outside the virial radius, r 200 , of the Milky Way (MW) or M31 which may have been within their virial boundaries in the past. More than half of all dwarfs at distances between one and two virial radii of each primary are backsplash galaxies. More distant backsplash systems, i.e., those that reach distances well beyond 2 r 200 , are typically systems close to apocentre of nearly radial orbits, and, therefore, essentially at rest relative to their primary. We use this result to investigate which LG dwarfs beyond ∼ 500 kpc of either primary could be a backsplash satellite of either MW or M31. The Tucana dwarf spheroidal (dSph), one of the few known quiescent LG field dwarfs, at d M31 ≈ 1350 kpc and d MW ≈ 880 kpc, is a promising candidate. Tucana's radial velocity suggests it is at rest relative to M31. Further, Tucana is located close to the orbital plane of M33 around M31, and simple orbit integrations indicate that Tucana may have been ejected during an early pericentric passage of M33 about ∼ 11 Gyr ago, a timing which approximately coincides with Tucana's last episode of star formation. We suggest that Tucana may have been a satellite of M31 or M33, providing a compelling explanation for its puzzling lack of gas and ongoing star formation despite its isolated nature.

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Tucana B: An Isolated and Quenched Ultra-faint Dwarf Galaxy at D=1.4 Mpc

Cited by 6 publications

References 0 publications

Astrophysical Tests of Dark Matter Self-Interactions

Astrophysical Tests of Dark Matter Self-Interactions

Discovery of a new Local Group Dwarf Galaxy Candidate in UNIONS: Boötes V

The Tucana dwarf spheroidal: a distant backsplash galaxy of M31?

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