Evidence of a Flat Outer Rotation Curve in a Star-bursting Disk Galaxy at z = 1.6

Drew, Patrick; Casey, Caitlin M.; Burnham, Anne D.; Hung, Chao-Ling; Kassin, Susan; Simons, Raymond C.; Zavala, Jorge A.

doi:10.3847/1538-4357/aaedbf

Cited by 24 publications

(25 citation statements)

References 70 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Also, this research would claim that "the dark matter cores" of the black holes shouldn't grow in mass any further, but they might change their gravitational geometry if more matter drops in the surface of the supermassive black hole and increases the time dilation at the center of it (although, black hole collisions might be an exception). That is also consistent with the observed behaviour of dark matter-we can see different shapes of dark matter halos [12] and relatively young galaxies with plenty of dark matter [13]. However, if we were to observe that dark matter halos are not more compact in very young galaxies on average when compared with old ones, we might also surmise that the hypothesis in this research is incorrect.…”

Section: Conclusion and Thoughtssupporting

confidence: 88%

Dark Matter: An Unforeseen Gravitational Property of Relativistic Space-Time?

Pukkila¹

2019

JHEPGC

View full text Add to dashboard Cite

If the wave functions of matter expanded with time dilation for an outside observer in the same way as photons do in gravitational redshift; with some modifications the general relativity might alone explain dark matter, galaxy rotation curves, and part of the energy released in supernova explosions. Also, the event horizons of black holes couldn't be formed when packing matter more and more densely together. Essentially, if the time dilation increases enough, the particles turn less localized to outside observers and the mass distribution of the same particles would expand into larger volume of space. Small particles deep inside a black hole might seem like dark matter instead by their gravitational influence if the time dilation alters their size enough for outside observers. At the same time, the surface particles of the black hole would be less dispersed, creating the Newtonian gravitational potential we see closer to black holes. The following research doesn't attempt to reformulate the general relativity itself, but only proposes the idea while approximating the Milky way gravity profile to compare the hypothesis with measurements. Therefore, actually proving the hypothesis is still far off while the idea is sound at its core.

show abstract

Section: Conclusion and Thoughtssupporting

confidence: 88%

Dark Matter: An Unforeseen Gravitational Property of Relativistic Space-Time?

Pukkila¹

2019

JHEPGC

View full text Add to dashboard Cite

show abstract

“…Moreover, Tiley et al (2019b) reported more than 50% dark matter fraction within 3.5 R e , which is similar to local star-forming disk galaxies (Persic et al 1996;Martinsson et al 2013;Courteau & Dutton 2015). Finally, another study by Drew et al (2018), analyzed a massive star-bursting galaxy at z = 1.55, showed strong evidence of flat RC between 6 − 14 kpc with 44% DM fraction within the effective radius.…”

Section: Introductionsupporting

confidence: 58%

Dark Matter Fraction in z~1 Star-Forming Galaxies

Sharma,

Salucci,

van de Ven

2021

Preprint

View full text Add to dashboard Cite

Context. The study of dark matter (DM) across the cosmic time-scales is essential for understanding the galaxy formation and evolution. Recent observational studies show that the further back in time (z > 0.5), rotation-supported star-forming galaxies (SFGs) begin to appear dark matter deficient compared to local SFGs. Aims. We present a observational study of the dark matter fraction in 225 rotation supported star-forming galaxies at z ≈ 0.9 having stellar mass range: 9.0 ≤ log(M * M ) ≤ 11.0 and star formation rate: 0.49 ≤ log S FR [M yr −1 ] ≤ 1.77. Methods. We study a sub-sample of the KMOS redshift one spectroscopic survey (KROSS) studied by Sharma et al. (2021). The stellar masses (M * ) of these objects were previously estimated using mass-to-light ratios derived from fitting the spectral energy distribution of the galaxies. Star formation rates were derived from the H α luminosities. The total gas masses (M gas ) are determined by scaling relations of molecular and atomic gas (Tacconi et al. 2018; Lagos et al. 2011, respectively). The dynamical masses (M dyn ) are directly derived from the rotation curves (RCs) at different scale lengths (effective radius: R e , ∼ 2 R e and ∼ 3 R e ) and then the dark matter fractions ( f DM = 1 − M bar /M dyn ) at these radii are calculated. Results. We report that at z ∼ 1 only a small fraction (∼ 5%) of our sample has a low (< 20%) DM fraction within ∼ 2-3 R e . The majority (> 72%) of SFGs in our sample have dark matter dominated outer disks (∼ 5 − 10 kpc) in agreement with local SFGs. Moreover, we find a large scatter in the fraction of dark matter at a given stellar mass (or circular velocity) with respect to local SFGs, suggesting that galaxies at z ∼ 1, a) span a wide range of stages in the formation of stellar disks, b) have diverse DM halo properties coupled with baryons.

show abstract

“…Source 850.95 was an outlier at 5.9 ± 3.3 kpc. It is known to be somewhat abnormally large as also traced by Hα kinematics (Drew et al 2018). Source 850.95 also has the lowest signal-tonoise ratio among our sources.…”

Section: Measuring Dust Sizes and Morphologymentioning

confidence: 64%

The Physical Drivers of the Luminosity-weighted Dust Temperatures in High-redshift Galaxies

Burnham

Casey

Zavala

et al. 2021

ApJ

Self Cite

View full text Add to dashboard Cite

The underlying distribution of galaxies' dust spectral energy distributions (SEDs) (i.e., their spectra reradiated by dust from rest-frame ∼3 μm to 3 mm) remains relatively unconstrained owing to a dearth of far-IR/(sub)millimeter data for large samples of galaxies. It has been claimed in the literature that a galaxy's dust temperature-observed as the wavelength where the dust SED peaks (λ peak )-is traced most closely by its specific star formation rate (sSFR) or parameterized "distance" to the SFR-M å relation (the galaxy "main sequence"). We present 0 24 resolved 870 μm ALMA dust continuum observations of seven z = 1.4-4.6 dusty star-forming galaxies chosen to have a large range of well-constrained luminosity-weighted dust temperatures. We also draw on similar-resolution dust continuum maps from a sample of ALESS submillimeter galaxies from Hodge et al (2016). We constrain the physical scales over which the dust radiates and compare those measurements to characteristics of the integrated SED. We confirm significant correlations of λ peak with both L IR (or SFR) and Σ IR (∝SFR surface density). We investigate the correlation between log 10 (λ peak ) and log 10 (Σ IR ) and find the relation to hold as would be expected from the Stefan-Boltzmann law, or the effective size of an equivalent blackbody. The correlations of λ peak with sSFR and distance from the SFR-M å relation are less significant than those for Σ IR or L IR ; therefore, we conclude that the more fundamental tracer of galaxies' luminosity-weighted integrated dust temperatures are indeed their star formation surface densities in line with local universe results, which relate closely to the underlying geometry of dust in the interstellar medium.

show abstract

Evidence of a Flat Outer Rotation Curve in a Star-bursting Disk Galaxy at z = 1.6

Cited by 24 publications

References 70 publications

Dark Matter: An Unforeseen Gravitational Property of Relativistic Space-Time?

Dark Matter: An Unforeseen Gravitational Property of Relativistic Space-Time?

Dark Matter Fraction in z~1 Star-Forming Galaxies

The Physical Drivers of the Luminosity-weighted Dust Temperatures in High-redshift Galaxies

Contact Info

Product

Resources

About