Observing Correlations Between Dark Matter Accretion and Galaxy Growth: I. Recent Star Formation Activity in Isolated Milky Way-Mass Galaxies

O'Donnell, Christine; Behroozi, Peter; More, Surhud

doi:10.48550/arxiv.2005.08995

Cited by 3 publications

(3 citation statements)

References 44 publications

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“…Although these fitting functions where obtained in [13] at fixed Γ, subsequent studies have shown that they evolve with redshift [16]. This is most likely due to the physics of mass accretion, which dominates mass growth at very high redshift [51][52][53][54]. Thus, we parametrise Γ as Γ(z) = Γ 1 + Γ 2 z.…”

Section: Dependence Of Hi Statistics On Splashback Radiusmentioning

confidence: 99%

The effect of finite halo size on the clustering of neutral hydrogen

Umeh,

Maartens,

Padmanabhan

et al. 2021

Preprint

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Post-reionisation 21cm intensity mapping experiments target the spectral line of neutral hydrogen (HI) resident in dark matter haloes. According to the halo model, these discrete haloes trace the continuous dark matter density field down to a certain scale, which is dependent on the halo physical size. The halo physical size defines an exclusion region which leaves imprints on the statistical properties of HI. We show how the effect of exclusion due to the finite halo size impacts the HI power spectrum, with the physical boundary of the host halo given by the splashback radius. Most importantly, we show that the white noise-like feature that appears in the zero-momentum limit of the power spectrum is exactly cancelled when the finite halo size is taken into consideration. This cancellation in fact applies to all tracers of dark matter density field, including galaxies. Furthermore, we show that the exclusion due to finite halo size leads to a sub-Poissonian noise signature on large scales, consistent with the results from N-body simulations.

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Section: Dependence Of Hi Statistics On Splashback Radiusmentioning

confidence: 99%

The effect of finite halo size on the clustering of neutral hydrogen

Umeh,

Maartens,

Padmanabhan

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…One scenario could be that the more massive halo has a larger gravitational potential and is able to cool hot accreted gas more efficiently for steady star formation, presented as the "hot-mode" accretion in Katz et al (2003) and Kereš et al (2005) or recycle earlier accreted hot gas easier (e.g. O'Donnell et al 2020). A second scenario could be that higher mass haloes contain more satellites, which could supply gas to their centrals via interactions and mergers in order to sustain their star formation (e.g.…”

Section: Trends In the Formation Timesmentioning

confidence: 99%

The Stellar Mass Assembly of Low Redshift, Massive, Central Galaxies in SDSS and the TNG300 simulation

Jackson,

Pasquali,

Pacifici

et al. 2020

Preprint

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The stellar mass assembly of galaxies can be affected by both secular and environmental processes. In this study, for the first time, we investigate the stellar mass assembly of ∼ 90, 000 low redshift, central galaxies selected from SDSS group catalogues (M Stellar 10 9.5 M , M Halo 10 12 M ) as a function of both stellar and halo mass. We use estimates of the times at which 10, 50 and 90 per cent of the stellar mass was assembled from photometric spectral energy distribution fitting, allowing a more complete investigation than single stellar ages alone. We consider trends in both stellar and halo mass simultaneously, finding dependencies of all assembly times on both. We find that galaxies with higher stellar masses (at constant halo mass) have on average older lookback times, similar to previous studies of galaxy assembly. We also find that galaxies at higher halo mass (at constant stellar mass) have younger lookback times, possibly due to a larger reservoir of gas for star formation. An exception to this is a sub sample with high stellar-to-halo mass ratios, which are likely massive, field spirals. We compare these observed trends to those predicted by the TNG300 simulation, finding good agreement overall as a function of either stellar or halo mass. However, some differences in the assembly times (of up to ∼ 3 Gyr) appear when considering both stellar and halo mass simultaneously, noticeably at intermediate stellar masses (M Stellar ∼ 10 11 M ). These discrepancies are possibly linked to the quenched fraction of galaxies and the kinetic mode AGN feedback implemented in TNG300.

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“…This, in turn, influences the formation of clusters and luminous galaxies. From a galaxy formation perspective, many recent studies have confirmed that MAR correlates with star formation and is therefore valuable in probing galaxy growth ★ E-mail: exhakaj@ucsc.edu (e.g., Diemer et al 2013;Wetzel & Nagai 2015;O'Donnell et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Beyond Mass: Detecting Secondary Halo Properties with Galaxy-Galaxy Lensing

Xhakaj,

Leauthaud,

Lange

et al. 2021

Preprint

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Secondary halo properties beyond mass, such as the mass accretion rate (MAR), concentration, and the half mass scale, are essential in understanding the formation of large-scale structure and dark matter halos. In this paper, we study the impact of secondary halo properties on the galaxy-galaxy lensing observable, ΔΣ. We build an emulator trained on N-body simulations to model ΔΣ and quantify the impact of different secondary parameters on the ΔΣ profile. We focus on the impact of MAR on ΔΣ. We show that a 3𝜎 detection of variations in MAR at fixed halo mass could be achieved with the Hyper Suprime Cam survey in combination with a proxy for MAR with scatter 𝜎 Γ dyn |obs < 1.5. We show that the full radial profile of ΔΣ depends on secondary properties at fixed halo mass. Consequently, an emulator that can perform full shape fitting yields better than 2 times improvement upon the constraints on MAR than only using the outer part of the halo. Finally, we highlight that miscentering and MAR impact the radial profile of ΔΣ in a similar fashion, implying that miscentering and MAR need to be modeled jointly for unbiased estimates of both effects. We show that present-day lensing data sets have the statistical capability to place constraints on halo MAR. Our analysis opens up new possibilities for observationally measuring the assembly history of the dark matter halos that host galaxies and clusters.

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Observing Correlations Between Dark Matter Accretion and Galaxy Growth: I. Recent Star Formation Activity in Isolated Milky Way-Mass Galaxies

Cited by 3 publications

References 44 publications

The effect of finite halo size on the clustering of neutral hydrogen

The effect of finite halo size on the clustering of neutral hydrogen

The Stellar Mass Assembly of Low Redshift, Massive, Central Galaxies in SDSS and the TNG300 simulation

Beyond Mass: Detecting Secondary Halo Properties with Galaxy-Galaxy Lensing

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