SDSS-IV MaNGA: spatial resolved properties of kinematically misaligned galaxies

Xu, Huizhong; Chen, Yanmei; Shi, Yong; Zhou, Yilong; Bizyaev, Dmitry; Bao, Min; Beom, Minje; Fernández-Trincado, José G.; Cao, Xiao

doi:10.1093/mnras/stac354

Cited by 16 publications

(19 citation statements)

References 76 publications

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“…High fractions of misaligned, i.e. not restricted to counter-rotating co-planar disks but in the range 30<Δ PA<150 degrees have also been reported in observational and simulation studies as a common kinematic characteristic for early type galaxies (Pizzella et al 2004;Davis et al 2011;Bryant et al 2019;Duckworth et al 2019;Duckworth, Tojeiro, & Kraljic 2020;Khim et al 2020;Xu et al 2022). We can estimate an upper limit to the fraction of gaseous counterrotators for the S0 class in our sample.…”

Section: The Frequency Of Counter-rotating Galaxiessupporting

confidence: 71%

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SDSS IV MaNGA: Characteristics of Edge-on Galaxies with a Counter-rotating Gaseous Disk

Beom,

Bizyaev,

Walterbos

et al. 2022

Preprint

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Counter-rotating components in galaxies are one of the most direct forms of evidence for past gas accretion or merging. We discovered ten edge-on disk gaseous counter-rotators in a sample of 523 edge-on galaxies identified in the final MaNGA (Mapping Nearby Galaxies at APO) IFU sample. The counter-rotators tend to located in small groups. The gaseous counter-rotators have intermediate stellar masses and and located in the green valley and red sequence of the color magnitude diagram. The average vertical extents of the stellar and ionized gas disks are the same as for the rest of the sample while their radial gas and stellar distributions are more centrally concentrated. This may point at angular momentum loss during the formation process of the counter-rotating disks. The counter-rotators have low gas and dust content, weak emission line strengths, and low star formation rates. This suggests that the formation of counter-rotators may be an efficient way to quench galaxies. One counter-rotator, SDSS J080016.09+292817.1 (Galaxy F), has a post starburst region and a possible AGN at the center. Another counter-rotator, SDSS J131234.03+482159.8 (Galaxy H), is identified as a potential on-going galaxy interaction with its companion satellite galaxy, a gas rich spiral galaxy. This may be representative case of a gaseous counter-rotator forming through a merger origin. However, tidal distortions expected in mergers are only found in a few of the galaxies and we cannot rule out direct gas accretion as another formation mechanism.

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Section: The Frequency Of Counter-rotating Galaxiessupporting

confidence: 71%

“…Li et al (2021) based on MaNGA (Mapping Nearby Galaxies at APO) MPL-8 (MaNGA Product Launches 8th version) identified hundreds of misalignment galaxies with morphological features indicating merging or interaction. In addition, Xu et al (2022) discuss the global characteristics of misalignment galaxies found in MaNGA MPL-10.…”

Section: Introductionmentioning

confidence: 99%

SDSS IV MaNGA: Characteristics of Edge-on Galaxies with a Counter-rotating Gaseous Disk

Beom,

Bizyaev,

Walterbos

et al. 2022

Preprint

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“…They show that the central starformation activity of SF misaligned galaxies is several times higher than the average of local SF galaxies within central 1kpc. Based on a larger sample, Xu et al (2022) discover that the central region of misaligned SF galaxies have higher sSFR in comparison with their control samples, and the misaligned galaxies shows smaller central D 𝑛 4000 indicating younger stellar populations in SF and GV misaligned galaxies. For the QS misaligned galaxies, the H and molecular gas deficiency could be due to a selection bias that progenitors with lower gaseous contents are easier to show kinematic misalignments, since the lack of interaction between accreted and pre-existing gas.…”

Section: Gaseous Contentmentioning

confidence: 89%

“…This is the largest gas-star kinematically misaligned sample so far. As a complementary work of Xu et al (2022), we study the global properties of the misaligned galaxies. The paper is organized as follows.…”

Section: Introductionmentioning

confidence: 99%

SDSS-IV MaNGA: global properties of kinematically misaligned galaxies

Zhou

Chen

Shi

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We select 456 gas-star kinematically misaligned galaxies from the internal Product Launch-10 of MaNGA survey, including 74 star-forming (SF), 136 green-valley (GV) and 206 quiescent (QS) galaxies. We find that the distributions of difference between gas and star position angles for galaxies have three local peaks at ∼0○, 90○, 180○. The fraction of misaligned galaxies peaks at log (M*/M⊙) ∼ 10.5 and declines to both low and high mass end. This fraction decreases monotonically with increasing SFR and sSFR. We compare the global parameters including gas kinematic asymmetry Vasym, H i detection rate and mass fraction of molecular gas, effective radius Re, Sérsic index n as well as spin parameter $\lambda _{R_e}$ between misaligned galaxies and their control samples. We find that the misaligned galaxies have lower H i detection rate and molecular gas mass fraction, smaller size, higher Sérsic index and lower spin parameters than their control samples. The SF and GV misaligned galaxies are more asymmetric in gas velocity fields than their controls. These observational evidences point to the gas accretion scenario followed by angular momentum redistribution from gas-gas collision, leading to gas inflow and central star formation for the SF and GV misaligned galaxies. We propose three possible origins of the misaligned QS galaxies: (1) external gas accretion; (2) merger; (3) GV misaligned galaxies evolve into QS galaxies.

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“…Similar to previous studies (Lagos et al 2015;Davis & Bureau 2016;Bryant et al 2019;Xu et al 2022), we assume that galaxies with a misalignment angle of less than 30 • are aligned, galaxies with 30 • < Ψ gas < 150 • are misaligned, and galaxies with 150 • < Ψ gas < 180 • could be considered to be counter-rotating. However, this cut-off is rather arbitrary, and in addition, the measurement errors (specifically PA kin for slow rotators) can be large, and the PAs are projected values, together resulting in an uncertainty on the Ψ gas misalignment.…”

Section: Misalignment Between Gas and Stars (ψ Gas )mentioning

confidence: 99%

Merger histories of brightest group galaxies from MUSE stellar kinematics

Loubser,

Lagos,

Babul

et al. 2022

Preprint

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Using Multi-Unit Spectroscopic Explorer (MUSE) spectroscopy, we analyse the stellar kinematics of 18 brightest group early-type (BGEs) galaxies, selected from the Complete Local-Volume Groups Sample (CLoGS). We analyse the kinematic maps for distinct features, and measure specific stellar angular momentum within one effective radius (λ e ). We classify the BGEs as fast (10/18) or slow (8/18) rotators, suggesting at least two different evolution paths. We quantify the anti-correlation between higherorder kinematic moment h 3 and V/σ (using the ξ 3 parameter), and the kinematic misalignment angle between the photometric and kinematic position angles (using the Ψ parameter), and note clear differences between these parameter distributions of the fast and slow rotating BGEs. We find that all 10 of our fast rotators are aligned between the morphological and kinematical axis, consistent with an oblate galaxy shape, whereas the slow rotators are spread over all three classes: oblate (1/8), triaxial (4/8), and prolate (3/8). We place the results into context using known radio properties, Xray properties, and observations of molecular gas. We find consistent merger histories inferred from observations for the fast-rotating BGEs, indicating that they experienced gas-rich mergers or interactions, and these are very likely the origin of the cold gas. Observational evidence for the slow rotators are consistent with gas-poor mergers. For the slow rotators with cold gas, all evidence point to cold gas cooling from the intragroup medium.

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SDSS-IV MaNGA: spatial resolved properties of kinematically misaligned galaxies

Cited by 16 publications

References 76 publications

SDSS IV MaNGA: Characteristics of Edge-on Galaxies with a Counter-rotating Gaseous Disk

SDSS IV MaNGA: Characteristics of Edge-on Galaxies with a Counter-rotating Gaseous Disk

SDSS-IV MaNGA: global properties of kinematically misaligned galaxies

Merger histories of brightest group galaxies from MUSE stellar kinematics

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