Study of the charged component in nuclear stimulated desorption

Kelson, I.; Nir, D.; Ringler, G; Haustein, P.E.

doi:10.1088/0022-3727/25/10/024

Cited by 33 publications

(47 citation statements)

References 4 publications

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“…The second technique estimates mass growth histories from measurements of the galaxy SMF using an evolving NDS criterion (Behroozi et al 2013). It is worthwhile to note that both techniques provide typical SFHs along with a rough indication of the scatter, but that individual galaxies may follow very different evolutionary pathways (Kelson 2014;Abramson et al 2015). We find that these two methods for deriving galaxy growth histories provide qualitatively similar results, but that they do disagree in detail.…”

Section: Discussionmentioning

confidence: 81%

THE SFR–M_* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

Tomczak

Quadri

Tran

et al. 2016

ApJ

320

492

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We explore star formation histories (SFHs) of galaxies based on the evolution of the star formation rate stellar mass relation (SFR-M * ). Using data from the FourStar Galaxy Evolution Survey (ZFOURGE) in combination with far-IR imaging from the Spitzer and Herschel observatories we measure the SFR-M * relation at 0.5 < z < 4. Similar to recent works we find that the average infrared spectral energy distributions of galaxies are roughly consistent with a single infrared template across a broad range of redshifts and stellar masses, with evidence for only weak deviations. We find that the SFR-M * relation is not consistent with a single power law of the form M SFR * µ a at any redshift; it has a power law slope of α ∼ 1 at low masses, and becomes shallower above a turnover mass (M 0 ) that ranges from 10 9.5 to 10 10.8 M e , with evidence that M 0 increases with redshift. We compare our measurements to results from state-of-the-art cosmological simulations, and find general agreement in the slope of the SFR-M * relation albeit with systematic offsets. We use the evolving SFR-M * sequence to generate SFHs, finding that typical SFRs of individual galaxies rise at early times and decline after reaching a peak. This peak occurs earlier for more massive galaxies. We integrate these SFHs to generate mass growth histories and compare to the implied mass growth from the evolution of the stellar mass function (SMF). We find that these two estimates are in broad qualitative agreement, but that there is room for improvement at a more detailed level. At early times the SFHs suggest mass growth rates that are as much as 10× higher than inferred from the SMF. However, at later times the SFHs under-predict the inferred evolution, as is expected in the case of additional growth due to mergers.

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Section: Discussionmentioning

confidence: 81%

THE SFR–M_* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

Tomczak

Quadri

Tran

et al. 2016

ApJ

320

492

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“…Several studies, however, have found a significant population of mergers (up to 20%) on the MS (Kartaltepe et al 2012;Hung et al 2013). In this scenario, the intrinsic scatter of the MS arises from the stochasticity in the gas accretion history 14 (Kelson 2014;Whitaker et al 2014).…”

Section: Implications For the Msmentioning

confidence: 99%

“…This underprediction may suggest that other processes, such as violent disk instability (e.g., Ceverino et al 2010;Porter et al 2014) may be an important source of outliers above the MS. It has also been suggested that the scatter of the MS may simply be a consequence of the central limit theorem if in situ star formation is a stochastic process (Kelson 2014). The approximately linear slope and the redshift evolution of the MS may therefore not be a useful constraint on theoretical models.…”

Section: Introductionmentioning

confidence: 99%

Variations of the Ism Compactness Across the Main Sequence of Star Forming Galaxies: Observations and Simulations

Martínez-Galarza

Smith

Lanz

et al. 2016

ApJ

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The majority of star-forming galaxies follow a simple empirical correlation in the star formation rate (SFR) versus stellar mass (M * ) plane, of the form M SFR * µ a , usually referred to as the star formation main sequence (MS). The physics that sets the properties of the MS is currently a subject of debate, and no consensus has been reached regarding the fundamental difference between members of the sequence and its outliers. Here we combine a set of hydro-dynamical simulations of interacting galactic disks with state-of-the-art radiative transfer codes to analyze how the evolution of mergers is reflected upon the properties of the MS. We present CHIBURST, a Markov Chain Monte Carlo spectral energy distribution (SED) code that fits the multi-wavelength, broad-band photometry of galaxies and derives stellar masses, SFRs, and geometrical properties of the dust distribution. We apply this tool to the SEDs of simulated mergers and compare the derived results with the reference output from the simulations. Our results indicate that changes in the SEDs of mergers as they approach coalescence and depart from the MS are related to an evolution of dust geometry in scales larger than a few hundred parsecs. This is reflected in a correlation between the specific star formation rate, and the compactness parameter , that parametrizes this geometry and hence the evolution of dust temperature (T dust ) with time. As mergers approach coalescence, they depart from the MS and increase their compactness, which implies that moderate outliers of the MS are consistent with late-type mergers. By further applying our method to real observations of luminous infrared galaxies (LIRGs), we show that the merger scenario is unable to explain these extreme outliers of the MS. Only by significantly increasing the gas fraction in the simulations are we able to reproduce the SEDs of LIRGs.

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“…For instance, the tight relation between M * and star formation rate (SFR) observed across a wide range of redshifts suggests that the starformation within galaxies is a highly regulated process (but see Kelson 2014 for an alternative point of view), and enhanced SFR during mergers has a small effect on the total mass-buildup of the galaxies (Noeske et al 2007b). The small intrinsic scatter of the fundamental plane of early-type galaxies sheds light on the variety of stellar populations of these galaxies (Prugniel & Simien 1996;Forbes et al 1998;Gargiulo et al 2009;Graves et al 2010;Taranu et al 2015).…”

Section: Introductionmentioning

confidence: 99%

“…Likewise, scatter in the M * −size relation appears to be small and constant since z ∼ 2 (van der Wel et al 2014), which provides constraints on simple dry merger models (Nipoti et al 2012). It is not known to what extent the scatter in these relations is due to different evolutionary pathways or to intrinsically stochastic processes (Kelson 2014).…”

Section: Introductionmentioning

confidence: 99%

Hierarchical Galaxy Growth and Scatter in the Stellar Mass–halo Mass Relation

Conroy

Behroozi

2016

ApJ

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The relation between galaxies and dark matter halos reflects the combined effects of many distinct physical processes. Observations indicate that the z = 0 stellar mass-halo mass (SMHM) relation has remarkably small scatter in stellar mass at fixed halo mass ( 0.2 dex) with little dependence on halo mass. We investigate the origins of this scatter by combining N-body simulations with observational constraints on the SMHM relation. We find that at the group and cluster scale (M vir > 10 14 M ⊙ ) the scatter due purely to hierarchical assembly is ≈ 0.16 dex, which is comparable to recent direct observational estimates. At lower masses, mass buildup since z ≈ 2 is driven largely by in-situ growth. We include a model for the in-situ buildup of stellar mass and find that an intrinsic scatter in this growth channel of 0.2 dex produces a relation between scatter and halo mass that is consistent with observations from 10 12 M ⊙ < M vir < 10 14.75 M ⊙ . The approximately constant scatter across a wide range of halo masses at z = 0 thus appears to be a coincidence as it is determined largely by in-situ growth at low masses and by hierarchical assembly at high masses. These results indicate that the scatter in the SMHM relation can provide unique insight into the regularity of the galaxy formation process.

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Study of the charged component in nuclear stimulated desorption

Cited by 33 publications

References 4 publications

THE SFR–M_* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

THE SFR–M_* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

Variations of the Ism Compactness Across the Main Sequence of Star Forming Galaxies: Observations and Simulations

Hierarchical Galaxy Growth and Scatter in the Stellar Mass–halo Mass Relation

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Study of the charged component in nuclear stimulated desorption

Cited by 33 publications

References 4 publications

THE SFR–M* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

THE SFR–M* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

Variations of the Ism Compactness Across the Main Sequence of Star Forming Galaxies: Observations and Simulations

Hierarchical Galaxy Growth and Scatter in the Stellar Mass–halo Mass Relation

Contact Info

Product

Resources

About

THE SFR–M_* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

THE SFR–M_* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*