New Constraints on the Origin of Surface Brightness Profile Breaks of Disk Galaxies from MaNGA

Tang, Yimeng; Chen, Qianhui; Zhang, Hong Xin; Lin, Zhoubin; Chen, Guangwen; Gao, Yongheng; Liang, Zhixiong; Liu, Haiyang; Kong, Xu

doi:10.3847/1538-4357/ab98fd

Cited by 8 publications

(23 citation statements)

References 67 publications

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“…Kennicutt 1989;Schaye 2004), and simulations of disc galaxies have found that the break may be a result of a star formation cutoff associated with a drop in cold gas density (Roškar et al 2008;Martínez-Serrano et al 2009;Sánchez-Blázquez et al 2009). This picture is consistent with the down-bending star-formation rate (SFR) profiles of Type II galaxies (Tang et al 2020). The radial position of the break has also been found to increase with cosmic time (Trujillo & Pohlen 2005;Azzollini et al 2008b) and galaxy mass (Pohlen & Trujillo 2006;Muñoz-Mateos et al 2013), consistent with inside-out growth of disc galaxies.…”

Section: Introductionsupporting

confidence: 80%

“…In Type II (truncated) galaxies, the break in the exponential light ★ E-mail: joel.pfeffer@icrar.org profile has been observed to coincide with a minimum in the colour, age and mass-to-light ratio profiles (Azzollini et al 2008a;Bakos et al 2008;Zheng et al 2015;Ruiz-Lara et al 2016). The breaks are largely absent in the mass profiles of Type II galaxies (Bakos et al 2008;Tang et al 2020) and are thus related to radial gradients in the stellar populations (similarly found in the simulations of Sánchez-Blázquez et al 2009). The disc breaks may result from star formation thresholds in the outer parts of galaxies (e.g.…”

Section: Introductionmentioning

confidence: 68%

“…Méndez-Abreu et al 2017), some general trends with galaxy mass and morphology are clear. With increasing galaxy mass, the fraction of Type I profiles decreases and the fraction of Type III profiles increases (Laine et al 2016;Tang et al 2020). The frequency of Type II galaxies increases with Hubble type (i.e.…”

Section: Introductionmentioning

confidence: 99%

“…The frequency of Type II galaxies increases with Hubble type (i.e. are more frequent in disc-dominated galaxies), while Type III profiles are more common in early-type galaxies (Pohlen & Trujillo 2006;Gutiérrez et al 2011;Laine et al 2016;Méndez-Abreu et al 2017;Tang et al 2020). Approximately 8 per cent of galaxies also have composite Type II+III profiles (Gutiérrez et al 2011).…”

Section: Introductionmentioning

confidence: 99%

“…Type III galaxies have been found to have upbending SFR profiles, though without strong radial gradients in the stellar populations (i.e. the surface brightness and mass profiles are closely related in Type III galaxies, Tang et al 2020). Borlaff et al (2018) found Type III break radius scaling relations are similar from 𝑧 = 0.6 to 𝑧 = 0, indicating a 'stable' formation process.…”

Section: Introductionmentioning

confidence: 99%

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Using the EAGLE simulations to elucidate the origin of disc surface brightness profile breaks as a function of mass and environment

Pfeffer,

Bekki,

Forbes

et al. 2021

Preprint

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We analyse the surface brightness profiles of disc-type galaxies in the EAGLE simulations in order to investigate the effects of galaxy mass and environment on galaxy profile types. Following observational works, we classify the simulated galaxies by their disc surface brightness profiles into single exponential (Type I), truncated (Type II) and anti-truncated (Type III) profiles. In agreement with previous observation and theoretical work, we find that Type II discs result from truncated star-forming discs that drive radial gradients in the stellar populations. In contrast, Type III profiles result from galaxy mergers, extended star-forming discs or the late formation of a steeper, inner disc. We find that the EAGLE simulations qualitatively reproduce the observed trends found between profile type frequency and galaxy mass, morphology and environment, such as the fraction of Type III galaxies increasing with galaxy mass, and the the fraction of Type II galaxies increasing with Hubble type. We investigate the lower incidence of Type II galaxies in galaxy clusters, finding, in a striking similarity to observed galaxies, that almost no S0-like galaxies in clusters have Type II profiles. Similarly, the fraction of Type II profiles for disc-dominated galaxies in clusters is significantly decreased relative to field galaxies. This difference between field and cluster galaxies is driven by star formation quenching. Following the cessation of star formation upon entering a galaxy cluster, the young stellar populations of Type II galaxies simply fade, leaving behind Type I galaxies.

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Section: Introductionsupporting

confidence: 80%

Section: Introductionmentioning

confidence: 68%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Using the EAGLE simulations to elucidate the origin of disc surface brightness profile breaks as a function of mass and environment

Pfeffer,

Bekki,

Forbes

et al. 2021

Preprint

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The AMIGA sample of isolated galaxies

Sánchez-Alarcón¹,

Román²,

Knapen³

et al. 2023

A&A

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Context. In the standard cosmological model of galaxy evolution, mergers and interactions play a fundamental role in shaping galaxies. Galaxies that are currently isolated are thus interesting because they allow us to distinguish between internal and external processes that affect the galactic structure. However, current observational limits may obscure crucial information in the low-mass or low-brightness regime. Aims. We use optical imaging of a subsample of the AMIGA catalogue of isolated galaxies to explore the impact of different factors on the structure of these galaxies. In particular, we study the type of disc break as a function of the degree of isolation and the presence of interaction indicators such as tidal streams or plumes, which are only detectable in the ultra-low surface brightness regime. Methods. We present ultra-deep optical imaging in the r band of a sample of 25 low-redshift (z < 0.035) isolated galaxies. Through careful data processing and analysis techniques, the nominal surface brightness limits achieved are comparable to those to be obtained on the ten-year LSST coadds (μr,lim ≳ 29.5 mag arcsec−2 [3σ; 10″ × 10″]). We place special emphasis on preserving the low surface brightness features throughout the processing. Results. The extreme depth of our imaging allows us to study the interaction signatures of 20 galaxies since Galactic cirrus is a strong limiting factor in the characterisation of interactions for the remaining 5 of them. We detect previously unreported interaction features in 8 (40% ± 14%) galaxies in our sample. We identify 9 galaxies (36% ± 10%) with an exponential disc (Type I), 14 galaxies (56% ± 10%) with a down-bending (Type II) profile, and only 2 galaxies (8% ± 5%) with up-bending (Type III) profiles. Isolated galaxies have considerably more purely exponential discs and fewer up-bending surface brightness profiles than field or cluster galaxies. We find clear minor merger activity in some of the galaxies with single exponential or down-bending profiles, and both of the galaxies with up-bending profiles show signatures of a past interaction. Conclusions. We show the importance of ultra-deep optical imaging in revealing faint external features in galaxies that indicate a probable history of interaction. We confirm that up-bending profiles are likely produced by major mergers, while down-bending profiles are probably formed by a threshold in star formation. Unperturbed galaxies that slowly evolve with a low star formation rate could induce the high rate of Type I discs in isolated galaxies.

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MUSE observations of the giant low surface brightness galaxy Malin 1: Numerous HII regions, star formation rate, metallicity, and dust attenuation

Junais,

Weilbacher,

Epinat

et al. 2024

A&A

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Context. Giant low surface brightness (GLSB) galaxies are an extreme class of objects with very faint and extended gas-rich disks. Malin 1 is the largest GLSB galaxy known to date and one of the largest individual spiral galaxies observed so far, but the properties and formation mechanisms of its giant disk are still poorly understood. Aims. We used VLT/MUSE IFU spectroscopic observations of Malin 1 to measure the star formation rate (SFR), dust attenuation, and gas metallicity within this intriguing galaxy. Methods. We performed a penalized pixel fitting modeling to extract emission line fluxes such as Hα, Hβ, [N II]6583 and [O III]5007 along the central region as well as from the extended disk of Malin 1. Results. Our observations reveal for the first time strong Hα emission distributed across numerous regions throughout the extended disk of Malin 1. The emission extends to radial distances of ∼100 kpc, which indicates recent star formation activity. We made an estimate of the dust attenuation in the disk of Malin 1 using the Balmer decrement and found that Malin 1 has a mean Hα attenuation of 0.36 mag. We observe a steep decline in the radial distribution of the SFR surface density (ΣSFR) within the inner 20 kpc, followed by a shallow decline in the extended disk. We estimated the gas phase metallicity in Malin 1. We also found for the first time that the metallicity shows a steep gradient from solar metallicity to subsolar values in the inner 20 kpc of the galaxy, followed by a flattening of the metallicity in the extended disk with a relatively high value of ∼0.6 Z⊙. We found that the normalized abundance gradient of the inner disk of Malin 1 is similar to the values found in normal galaxies. However, the normalized gradient observed in the outer disk can be considered extreme when compared to other disk galaxies. A comparison of the SFR surface density and gas surface density shows that unlike normal disk galaxies or other low surface brightness galaxies, the outer disk of Malin 1 exhibits a relatively low star formation efficiency based on atomic gas-mass estimates, which may be mildly exacerbated by the vanishing upper molecular gas-mass limits found by recent CO studies. Conclusions. With the detection of emission lines in a large part of the extended disk of Malin 1, this work sheds light on the star formation processes in this unique galaxy, highlighting its extended star-forming disk, dust attenuation, almost flat metallicity distribution in the outer disk, and exceptionally low star formation efficiency. Together with previous results, our findings contribute to a more detailed understanding of the formation of the giant disk of Malin 1, and they also constrain possible proposed scenarios of the nature of GLSB galaxies in general.

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New Constraints on the Origin of Surface Brightness Profile Breaks of Disk Galaxies from MaNGA

Cited by 8 publications

References 67 publications

Using the EAGLE simulations to elucidate the origin of disc surface brightness profile breaks as a function of mass and environment

Using the EAGLE simulations to elucidate the origin of disc surface brightness profile breaks as a function of mass and environment

The AMIGA sample of isolated galaxies

MUSE observations of the giant low surface brightness galaxy Malin 1: Numerous HII regions, star formation rate, metallicity, and dust attenuation

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