A new algorithm to quantify maximum discs in galaxies

Starkman, Nathaniel; Lelli, Federico; McGaugh, Stacy S.; Schombert, James M.

doi:10.1093/mnras/sty2011

Cited by 21 publications

(22 citation statements)

References 41 publications

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“…Neglecting measurements with large uncertainties, ∼ 90% of the bars are consistent with the fast regime at 95% confident level. These galaxies should host little DM in their central regions, in agreement with the findings based on the study of rotation curves for unbarred galaxies (Debattista & Sellwood 2000;Starkman et al 2018).…”

Section: Introductionsupporting

confidence: 88%

“…The slow down of the bar is stronger if a massive and centrally-concentrated DM halo is present, because there is more mass ready to absorb angular momentum near the resonances and dynamical friction is more efficient (see Athanassoula 2014 andSellwood 2014, for further discussion). This implies that galaxies hosting fast bars should be embedded in DM halos with a low central density, such as those required in the maximum disc hypothesis (Debattista & Sellwood 2000;Palunas & Williams 2000;Fuchs 2001;Starkman et al 2018). Nevertheless, other galaxy properties may influence the angular momentum exchange within the galaxy, such as the halo triaxiality, presence of gas, and disc velocity dispersion (Athanassoula 2003;Athanassoula et al 2013).…”

Section: Introductionmentioning

confidence: 99%

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Bar pattern speeds in CALIFA galaxies III. Solving the puzzle of ultrafast bars

Cuomo,

Lee,

Buttitta

et al. 2021

Preprint

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Context. More than 10% of the barred galaxies with a direct measurement of the bar pattern speed host an ultrafast bar. These bars extend well beyond the corotation radius and challenge our understanding of the orbital structure of barred galaxies. Most of them are found in spiral galaxies, rather than in lenticular ones. Aims. We analysed the properties of the ultrafast bars detected in the Calar Alto Legacy Integral Field Spectroscopy Area Survey to investigate whether they are an artefact resulting from an overestimation of the bar radius and/or an underestimation of the corotation radius or a new class of bars, whose orbital structure has not yet been understood. Methods. We revised the available measurements of the bar radius based on ellipse fitting and Fourier analysis and of the bar pattern speed from the Tremaine-Weinberg method. In addition, we measured the bar radius from the analysis of the maps tracing the transverse-to-radial force ratio, which we obtained from the deprojected i-band images of the galaxies retrieved from the Sloan Digital Sky Survey. Results. We found that nearly all the sample galaxies are spirals with an inner ring or pseudo-ring circling the bar and/or strong spiral arms, which hamper the measurement of the bar radius from the ellipse fitting and Fourier analysis. According to these methods, the bar ends overlap the ring or the spiral arms making the adopted bar radius unreliable. On the contrary, the bar radius from the ratio maps are shorter than the corotation radius. This is in agreement with the theoretical predictions and findings of numerical simulations about the extension and stability of the stellar orbits supporting the bars. Conclusions. We conclude that ultrafast bars are no longer observed when the correct measurement of the bar radius is adopted. Deriving the bar radius in galaxies with rings and strong spiral arms is not straightforward and a solid measurement method based on both photometric and kinematic data is still missing.

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Section: Introductionsupporting

confidence: 88%

Section: Introductionmentioning

confidence: 99%

Bar pattern speeds in CALIFA galaxies III. Solving the puzzle of ultrafast bars

Cuomo,

Lee,

Buttitta

et al. 2021

Preprint

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“…In our computation, we fix the total gas mass to match the total mass inferred from the photometry and vary the stellar mass-to-light ratio of the disk from ϒ d ¼ 0 up to larger values that saturate the observed kinematic velocity [61]. In Fig.…”

Section: Application: Low-surface Brightness Sparc Galaxiesmentioning

confidence: 99%

Ultralight dark matter in disk galaxies

et al. 2019

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Analytic arguments and numerical simulations show that bosonic ultralight dark matter (ULDM) would form cored density distributions ("solitons") at the center of galaxies. ULDM solitons offer a promising way to exclude or detect ULDM by looking for a distinctive feature in the central region of galactic rotation curves. Baryonic contributions to the gravitational potential pose an obstacle to such analyses, being (i) dynamically important in the inner galaxy and (ii) highly nonspherical in rotation-supported galaxies, resulting in nonspherical solitons. We present an algorithm for finding the ground-state soliton solution in the presence of stationary nonspherical background baryonic mass distribution. We quantify the impact of baryons on the predicted ULDM soliton in the Milky Way and in low-surface-brightness galaxies from the SPARC database.

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“…( 1)). Here we adjust their values to achieve a maximum-disk fit (van Albada & Sancisi 1986;Starkman et al 2018), ensuring that the inner part of the observed rotation curve is fully explained by luminous matter. Our fits can be seen in Fig.…”

Section: Maximum-disk Mass Modelsmentioning

confidence: 99%

From spirals to lenticulars: Evidence from the rotation curves and mass models of three early-type galaxies

Shelest

Lelli

2020

A&A

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Rotation curves have traditionally been difficult to trace for early-type galaxies (ETGs) because they often lack a high-density disk of cold gas as in late-type galaxies (LTGs). In this work, we derive rotation curves for three lenticular galaxies from the ATLAS3D survey, combining CO data in the inner parts with deep HI data in the outer regions, extending out to 10−20 effective radii. We also use Spitzer photometry at 3.6 μm to decompose the rotation curves into the contributions of baryons and dark matter (DM). We find that (1) the rotation-curve shapes of these ETGs are similar to those of LTGs of a similar mass and surface brightness; (2) the dynamically-inferred stellar mass-to-light ratios are small for quiescent ETGs but similar to those of star-forming LTGs; (3) the DM halos follow the same scaling relations with galaxy luminosity as those of LTGs; and (4) one galaxy (NGC 3626) is poorly fit by cuspy DM profiles, suggesting that DM cores may exist in high-mass galaxies too. Our results indicate that these lenticular galaxies have recently transitioned from LTGs to ETGs without altering their DM halo structure (e.g., via a major merger), and they could be faded spirals. We also confirm that ETGs follow the same radial acceleration relation as LTGs, reinforcing the notion that this is a universal law for all galaxy types.

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A new algorithm to quantify maximum discs in galaxies

Cited by 21 publications

References 41 publications

Bar pattern speeds in CALIFA galaxies III. Solving the puzzle of ultrafast bars

Bar pattern speeds in CALIFA galaxies III. Solving the puzzle of ultrafast bars

Ultralight dark matter in disk galaxies

From spirals to lenticulars: Evidence from the rotation curves and mass models of three early-type galaxies

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