On the surface density of dark matter haloes

Saburova, Anna S.; Popolo, A. Del

doi:10.1093/mnras/stu1957

Cited by 44 publications

(36 citation statements)

References 142 publications

(213 reference statements)

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“…12 -14 I plot the dark halo central densities, radial scales and masses within optical borders against the disc sizes. Squares show the compilation of literature data on the dark halo parameters from Saburova & Del Popolo (2014), which also contains three giant LSB galaxies Malin 1, Malin 2 and NGC7589 for piso dark halo. Diamonds demonstrate the data from the current paper.…”

Section: Discussionmentioning

confidence: 99%

What made discy galaxies giant?

Saburova

2017

Monthly Notices of the Royal Astronomical Society

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I studied giant discy galaxies with optical radii more than 30 kpc. The comparison of these systems with discy galaxies of moderate sizes revealed that they tend to have higher rotation velocities, B-band luminosities, H masses and dark-to-luminous mass ratios. The giant discs follow the trend log(M HI )(R 25 ) found for normal size galaxies. It indicates the absence of the peculiarities of evolution of star formation in these galaxies. The H mass to luminosity ratio of giant galaxies appears not to differ from that of normal size galaxies, giving evidences in favor of similar star formation efficiency. I also found that the bars and rings occur more frequently among giant discs. I performed mass-modelling of the subsample of 18 giant galaxies with available rotation curves and surface photometry data and constructed χ 2 maps for the parameters of their dark matter haloes. These estimates indicate that giant discs tend to be formed in larger more massive and rarified dark haloes in comparison to moderate size galaxies. However giant galaxies do not deviate significantly from the relations between the optical sizes and dark halo parameters for moderate size galaxies. These findings can rule out the catastrophic scenario of the formation of at least most of giant discs, since they follow the same relations as normal discy galaxies. The giant sizes of the discs can be due to the high radial scale of the dark matter haloes in which they were formed.

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Section: Discussionmentioning

confidence: 99%

What made discy galaxies giant?

Saburova

2017

Monthly Notices of the Royal Astronomical Society

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“…Figure 6. The radial gradient of the oxygen abundance taken from Pilyugin, Grebel, & Kniazev (2014) (filled circles) and PT2005 (open triangles) compared to the dark halo to stellar mass ratio within optical borders (Saburova & Del Popolo 2014). The line denotes the linear regression.…”

Section: Discussionmentioning

confidence: 99%

“…Since the behavior of y ef f beyond the optical borders is not known, it is worth trying to compare y ef f,max with the dark halo mass M halo inside of optical radius R 25 , using the estimates of M halo compiled in Saburova & Del Popolo (2014). The results are given in Fig.…”

Section: On the Relation Between Maximal Oxygen Yield Dark Halo And mentioning

confidence: 99%

“…The relation between the dark halo mass fraction and O/H radial gradient Since a halo mass influence the chemical evolution of gas in a disk, we checked whether there is a connection between the dark halo mass fraction and the radial distribution of metallicity. For this purpose we used a larger statistics than we did above, taking the sample of galaxies with available measurements of metallicity gradients from Pilyugin, Grebel, & Kniazev (2014) and the dark halo masses from Saburova & Del Popolo (2014). Note that the metallicity gradient is less sensitive to the calibration uncertainty than the values of O/H.…”

Section: On the Relation Between Maximal Oxygen Yield Dark Halo And mentioning

confidence: 99%

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On the Effective Oxygen Yield in the Disks of Spiral Galaxies

Засов¹,

Saburova²,

Abramova³

2015

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The factors influencing chemical evolution of galaxies are poorly understood. Both gas inflow and gas outflow reduce a gas-phase abundance of heavy elements (metallicity) whereas the ongoing star formation continuously increases it. To exclude the stellar nucleosynthesis from consideration, we analyze for the sample of 14 spiral galaxies the radial distribution of the effective yield of oxygen y ef f , which would be identical to the true stellar yield (per stellar generation) y o if the evolution followed the closed box model. As the initial data for gas-phase abundance we used the O/H radial profiles from Moustakas, Kennicutt, Tremonti et al. (2010) In most of galaxies with the PT2005 calibration, which we consider as a preferred one, the yield y ef f in the main disk (R ≥ 0.2 R 25 , where R 25 is the optical radius) increases with radius, remaining lower than the empirically found true stellar yield y o . This may indicate the inflow of low-enriched gas predominantly to the inner disk regions, which reduces y ef f . We show that the maximal values of the effective yield in the main disks of galaxies, y ef f,max , anti-correlate with the total mass of galaxies and with the mass of their dark halo enclosed within R 25 . It allows to propose the higher role of gas accretion for galaxies with massive halos. We also found that the radial gradient of oxygen abundance normalized to R 25 has a tendency to be shallower in the systems with lower dark halo to stellar mass ratio within the optical radius, which, if confirmed, gives evidences of the effective radial mixing of gas in galaxies with the relatively light dark matter halo.

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“…In Fig. 32 the dark halo mass within the optical limits is matched with the galaxy morphological type according to paper [298]. The morphological type is given in the numerical coding by de Vaucouleurs (types S0, Sa, Sb, Sc, Sd and Irr correspond to t = −1, 1, 3, 5, 7 and > 7 ).…”

Section: Dark Matter and Morphological Type Of Galaxymentioning

confidence: 99%

Dark matter in galaxies

Засов¹,

Saburova²,

Хоперсков³

et al. 2017

Phys.-Usp.

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Dark matter in galaxies, its abundance, and its distribution remain a subject of long-standing discussion, especially in view of the fact that neither dark matter particles nor dark matter bodies have yet been found. Experts' opinions range from a very large number of completely dark galaxies exist to nonbaryonic dark matter does not exist at all in any significant amounts. We discuss astronomical evidence for the existence of dark matter and its connection with visible matter and examine attempts to estimate its mass and distribution in galaxies from photometry, dynamics, gravitational lensing, and other observations (the cosmological aspects of the existence of dark matter are not considered in this review). In our view, the presence of dark matter in and around galaxies is a well-established fact. We conclude with an overview of mechanisms by which a dark halo can influence intragalactic processes.Comment: 82 pages, 35 figure

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On the surface density of dark matter haloes

Cited by 44 publications

References 142 publications

What made discy galaxies giant?

What made discy galaxies giant?

On the Effective Oxygen Yield in the Disks of Spiral Galaxies

Dark matter in galaxies

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