Galaxy formation and evolution science in the era of the Large Synoptic Survey Telescope

Robertson, Brant; Banerji, M.; Brough, Sarah; Davies, Roger L.; Ferguson, Henry C.; Hausen, Ryan; Kaviraj, Sugata; Newman, Jeffrey A.; Schmidt, Samuel J.

doi:10.1038/s42254-019-0067-x

Cited by 26 publications

(19 citation statements)

References 186 publications

(198 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…the ones visible in Figure 11) are faint with surface brightnesses typically fainter than 29 mag arcsec −2 . This suggests that finding large samples of DM deficient candidates would ideally require deep wide-area surveys, such as LSST (Robertson et al 2019;Kaviraj 2020), which have limiting surface-brightnesses that are fainter than such values.…”

Section: Formation Of Dm Deficient Galaxies Through Stripping Of Dm Imentioning

confidence: 99%

See 1 more Smart Citation

Dark matter-deficient dwarf galaxies form via tidal stripping of dark matter in interactions with massive companions

Jackson

Kaviraj

Martin

et al. 2021

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

In the standard ΛCDM (Lambda cold dark matter) paradigm, dwarf galaxies are expected to be dark matter-rich, as baryonic feedback is thought to quickly drive gas out of their shallow potential wells and quench star formation at early epochs. Recent observations of local dwarfs with extremely low dark matter content appear to contradict this picture, potentially bringing the validity of the standard model into question. We use NewHorizon, a high-resolution cosmological simulation, to demonstrate that sustained stripping of dark matter, in tidal interactions between a massive galaxy and a dwarf satellite, naturally produces dwarfs that are dark matter-deficient, even though their initial dark matter fractions are normal. The process of dark matter stripping is responsible for the large scatter in the halo-to-stellar mass relation in the dwarf regime. The degree of stripping is driven by the closeness of the orbit of the dwarf around its massive companion and, in extreme cases, produces dwarfs with halo-to-stellar mass ratios as low as unity, consistent with the findings of recent observational studies. ∼30 per cent of dwarfs show some deviation from normal dark matter fractions due to dark matter stripping, with 10 per cent showing high levels of dark matter deficiency (Mhalo/M⋆ < 10). Given their close orbits, a significant fraction of dark matter-deficient dwarfs merge with their massive companions (e.g. ∼70 per cent merge over time-scales of ∼3.5 Gyr), with the dark matter-deficient population being constantly replenished by new interactions between dwarfs and massive companions. The creation of these galaxies is therefore a natural by-product of galaxy evolution and their existence is not in tension with the standard paradigm.

show abstract

Section: Formation Of Dm Deficient Galaxies Through Stripping Of Dm Imentioning

confidence: 99%

“…The cosmological volume enables us to probe galaxy populations in a statistical manner, taking into account environmental effects (which idealised studies, for instance, cannot do), and is particularly important for making meaningful comparisons to large observational surveys (e.g. forthcoming datasets like LSST, Robertson et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Dark matter-deficient dwarf galaxies form via tidal stripping of dark matter in interactions with massive companions

Jackson

Kaviraj

Martin

et al. 2021

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

show abstract

“…It would therefore be informative to perform a similar study at higher redshifts. This would require high resolution imaging over a large area of the sky to be able to derive the morphological parameters from the image plane for a statistically large sample of galaxies in a range of environments, for example with the Vera C. Rubin Observatory (Robertson et al 2019). B.1.…”

Section: Discussionmentioning

confidence: 99%

Galaxy and Mass Assembly: Group and field galaxy morphologies in the star-formation rate – stellar mass plane

Pearson

Wang

Brough

et al. 2021

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We study the environment in which a galaxy lies (i.e. field or group) and its connection with the morphology of the galaxy. This is done by examining the distribution of parametric and non-parametric statistics across the star-formation rate (SFR) – stellar mass (M⋆) plane and studying how these distributions change with the environment in the local universe (z < 0.15). Methods. We determine the concentration (C), Gini, M20, asymmetry, Gini-M20 bulge statistic (GMB), 50% light radius (r50), total Sérsic index, and bulge Sérsic index (nBulge) for galaxies from the Galaxy and Mass Assembly (GAMA) survey using optical images from the Kilo Degree Survey. We determine the galaxy environment using the GAMA group catalogue and split the galaxies into field or group galaxies. The group galaxies are further divided by the group halo mass (Mh)−11 ≤ log(Mh/M⊙) < 12, 12 ≤ log(Mh/M⊙) < 13, and 13 ≤ log(Mh/M⊙) < 14 – and into central and satellite galaxies. The galaxies in each of these samples are then placed onto the SFR-M⋆ plane, and each parameter is used as a third dimension. We fit the resulting distributions for each parameter in each sample using two two-dimensional Gaussian distributions: one for star-forming galaxies and one for quiescent galaxies. The coefficients of these Gaussian fits are then compared between environments. Results. Using C and r50, we find that galaxies typically become larger as the group mass increases. This change is greater for larger galaxies. There is no indication that galaxies are typically more or less clumpy as the environment changes. Using GMB and nBulge, we see that the star-forming galaxies do not become more bulge or disk dominated as the group mass changes. Asymmetry does not appear to be greatly influenced by environment.

show abstract

“…UDGs are, therefore, a normal component of the dwarf galaxy population at low surface brightnesses. Note that since NewHorizon does not contain any clusters, a clear prediction is that UDGs should exist in large numbers in groups and the field and should be routinely detectable in new and future deep surveys such as the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP Aihara et al 2019) and the Legacy Survey of Space and time (LSST) on the Vera C. Rubin Observatory (Robertson et al 2019). In Figure 2 we present mock images of typical galaxies that occupy different regions of the locus, created using the SKIRT9 code (Baes & Camps 2015), which employs full radiative transfer based on the stars and gas within a galaxy.…”

Section: The Surface Brightness Vs Stellar Mass Plane In the Nearby mentioning

confidence: 99%

The origin of low-surface-brightness galaxies in the dwarf regime

Jackson

Martin

Kaviraj

et al. 2021

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

Low-surface-brightness galaxies (LSBGs) – defined as systems that are fainter than the surface-brightness limits of past wide-area surveys – form the overwhelming majority of galaxies in the dwarf regime (M⋆ < 109 M⊙). Using NewHorizon, a high-resolution cosmological simulation, we study the origin of LSBGs and explain why LSBGs at similar stellar mass show the large observed spread in surface brightness. NewHorizon galaxies populate a well-defined locus in the surface brightness – stellar mass plane, with a spread of ∼3 mag arcsec−2, in agreement with deep SDSS Stripe data. Galaxies with fainter surface brightnesses today are born in regions of higher dark-matter density. This results in faster gas accretion and more intense star formation at early epochs. The stronger resultant supernova feedback flattens gas profiles at a faster rate which, in turn, creates shallower stellar profiles (i.e. more diffuse systems) more rapidly. As star formation declines towards late epochs (z < 1), the larger tidal perturbations and ram pressure experienced by these systems (due to their denser local environments) accelerate the divergence in surface brightness, by increasing their effective radii and reducing star formation respectively. A small minority of dwarfs depart from the main locus towards high surface brightnesses, making them detectable in past wide surveys (e.g. standard-depth SDSS images). These systems have anomalously high star-formation rates, triggered by recent, fly-by or merger-driven starbursts. We note that objects considered extreme/anomalous at the depth of current datasets, e.g. ‘ultra-diffuse galaxies’, actually dominate the predicted dwarf population and will be routinely visible in future surveys like LSST.

show abstract

Galaxy formation and evolution science in the era of the Large Synoptic Survey Telescope

Cited by 26 publications

References 186 publications

Dark matter-deficient dwarf galaxies form via tidal stripping of dark matter in interactions with massive companions

Dark matter-deficient dwarf galaxies form via tidal stripping of dark matter in interactions with massive companions

Galaxy and Mass Assembly: Group and field galaxy morphologies in the star-formation rate – stellar mass plane

The origin of low-surface-brightness galaxies in the dwarf regime

Contact Info

Product

Resources

About