The stellar host in star-forming low-mass galaxies: Evidence for two classes

Lumbreras-Calle, Alejandro; Méndez-Abreu, J.; Muñoz–Tuñón, C.

doi:10.1051/0004-6361/201935288

Cited by 3 publications

(3 citation statements)

References 89 publications

(93 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In general cases, galaxies have been found to be more compact and smaller at longer wavelengths. For early-type galaxies or classical bulges observed through optical-NIR channels (approximately from u-K s bands), the Sérsic index increases with wavelength, but the variations are shallow or flat (n ∼ 3-4; Kelvin et al 2012;Vika et al 2013;Vulcani et al 2014;Lange et al 2015;Marian et al 2018;Lima-Dias et al 2021); in the same wavelength range, late-type galaxies or disks appears invariable in concentration level (commonly with the Sérsic index n ∼ 1; Kelvin et al 2012;Vulcani et al 2014;Lumbreras-Calle et al 2019;Lima-Dias et al 2021). When observed at UV bands (λ < 3000 Å), earlytype galaxies or classical bulges appear with lower values for the Sérsic index (n ∼ 2-3; Rampazzo et al 2017;Leahy et al 2023).…”

Section: Comparison With Other Workmentioning

confidence: 99%

Multiwavelength Bulge–Disk Decomposition for the Galaxy M81 (NGC 3031). I. Morphology

Gong

Mao

Gao

et al. 2023

ApJS

View full text Add to dashboard Cite

A panchromatic investigation of morphology for the early-type spiral galaxy M81 is presented in this paper. We perform bulge–disk decomposition in M81 images at a total of 20 wave bands from far-UV to near-IR (NIR) obtained with GALEX, Swift, Sloan Digital Sky Survey, WIYN, Two Micron All Sky Survey, Wide-field Infrared Survey Explorer, and Spitzer. Morphological parameters such as Sérsic index, effective radius, position angle, and axis ratio for the bulge and the disk are thus derived at all of the wave bands, which enables quantifying the morphological K-correction for M81 and makes it possible to reproduce images for the bulge and the disk in the galaxy at any wave band. The morphology as a function of wavelength appears as a variable-slope trend of the Sérsic index and the effective radius, in which the variations are steep at UV–optical and shallow at optical–NIR bands; the position angle and the axis ratio keep invariable at least at optical–NIR bands. It is worth noting that the Sérsic index for the bulge reaches ∼4–5 at optical and NIR bands, but drops to ∼1 at UV bands. This difference brings forward a caveat that a classical bulge is likely misidentified for a pseudobulge or no bulge at high redshifts where galaxies are observed through rest-frame UV channels with optical telescopes. The next work of this series is planned to study spatially resolved spectral energy distributions for the bulge and the disk, respectively, and thereby explore stellar population properties and star formation/quenching history for the galaxy composed of the subsystems.

show abstract

Section: Comparison With Other Workmentioning

confidence: 99%

Multiwavelength Bulge–Disk Decomposition for the Galaxy M81 (NGC 3031). I. Morphology

Gong

Mao

Gao

et al. 2023

ApJS

View full text Add to dashboard Cite

show abstract

“…In contrast, narrowband photometric surveys such as HiZELS (Best et al 2013;Sobral et al 2013;Matthee et al 2017), ALHAMBRA (Moles et al 2008;Molino et al 2014), DAWN (Coughlin et al 2018), J-PLUS (Cenarro et al 2019), S-PLUS (Mendes de Oliveira et al 2019), the Deep and UDeep layers driven by the Subaru Strategic Program with the Hyper Suprime-Cam (HSC-SSP) (Hayashi et al 2018(Hayashi et al , 2020, LAGER (Khostovan et al 2020), or SHARDS (Pérez-González et al 2013Lumbreras-Calle et al 2019), experience these effects to a lesser degree. In particular, narrowband photometric surveys are able to detect fainter objects than their spectroscopic counterpart at a fixed exposure time.…”

Section: Introductionmentioning

confidence: 99%

The miniJPAS survey: Identification and characterization of the emission line galaxies down toz< 0.35 in the AEGIS field

Martínez-Solaeche¹,

Delgado²,

García-Benito³

et al. 2022

A&A

View full text Add to dashboard Cite

The Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) is expected to map thousands of square degrees of the northern sky with 56 narrowband filters (spectral resolution of R ∼ 60) in the upcoming years. This resolution allows us to study emission line galaxies (ELGs) with a minimum equivalent width of 10 Å in the Hα emission line for a median signal-to-noise ratio (S/N) of 5. This will make J-PAS a very competitive and unbiased emission line survey compared to spectroscopic or narrowband surveys with fewer filters. The miniJPAS survey covered 1 deg2, and it used the same photometric system as J-PAS, but the observations were carried out with the pathfinder J-PAS camera. In this work, we identify and characterize the sample of ELGs from miniJPAS with a redshift lower than 0.35, which is the limit to which the Hα line can be observed with the J-PAS filter system. Using a method based on artificial neural networks, we detect the ELG population and measure the equivalent width and flux of the Hα, Hβ, [O III], and [N II] emission lines. We explore the ionization mechanism using the diagrams [OIII]/Hβ versus [NII]/Hα (BPT) and EW(Hα) versus [NII]/Hα (WHAN). We identify 1787 ELGs (83%) from the parent sample (2154 galaxies) in the AEGIS field. For the galaxies with reliable EW values that can be placed in the WHAN diagram (2000 galaxies in total), we obtained that 72.8 ± 0.4%, 17.7 ± 0.4%, and 9.4 ± 0.2% are star-forming (SF), active galactic nucleus (Seyfert), and quiescent galaxies, respectively. The distribution of EW(Hα) is well correlated with the bimodal color distribution of galaxies. Based on the rest-frame (u − r)–stellar mass diagram, 94% of the blue galaxies are SF galaxies, and 97% of the red galaxies are LINERs or passive galaxies. The nebular extinction and star formation rate (SFR) were computed from the Hα and Hβ fluxes. We find that the star formation main sequence is described as log SFR [M⊙ yr−1] = 0.90−0.02+0.02 log M⋆[M⊙]−8.85−0.20+0.19 and has an intrinsic scatter of 0.20−0.01+0.01. The cosmic evolution of the SFR density (ρSFR) is derived at three redshift bins: 0 < z ≤ 0.15, 0.15 < z ≤ 0.25, and 0.25 < z ≤ 0.35, which agrees with previous results that were based on measurements of the Hα emission line. However, we find an offset with respect to other estimates that were based on the star formation history obtained from fitting the spectral energy distribution of the stellar continuum. We discuss the origin of this discrepancy, which is probably a combination of several factors: the escape of ionizing photons, the SFR tracers, and dust attenuation, among others.

show abstract

“…The emergence of medium-and narrow-band photometric surveys continuously covering a large wavelength range, such as the Subaru Cosmic Evolution Survey 20 (Subaru COS-MOS 20; Taniguchi et al 2015;Sobral et al 2018), the Advance Large Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) survey (Moles et al 2008), the National Optical Astronomy Observatory (NOAO) Extremely Wide-Field Infrared Imager (NEWFIRM) Medium-Band Survey (NMBS; van Dokkum et al 2009), the Survey for High-z Absorption Red and Dead Sources (SHARDS; Pérez-González et al 2013), the Physics of the Accelerating Universe Survey (PAUS; Eriksen et al 2019), and the Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS; Benitez et al 2014), is progressively changing this picture. Multi-band photometric surveys have reached high enough spectral resolution to first detect broad emission lines (Chaves-Montero et al 2017;Lumbreras-Calle et al 2019) and then detect narrow lines and approximately resolve the profile of broad lines (Alarcon et al 2021;Martínez-Solaeche et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Black hole virial masses from single-epoch photometry

Chaves-Montero¹,

Bonoli²,

Trakhtenbrot³

et al. 2022

A&A

View full text Add to dashboard Cite

Context. Precise measurements of black hole masses are essential to understanding the coevolution of these sources and their host galaxies. Aims. We develop a novel approach for computing black hole virial masses using measurements of continuum luminosities and emission line widths from partially overlapping, narrow-band observations of quasars; we refer to this technique as single-epoch photometry. Methods. This novel method relies on forward-modelling quasar observations for estimating emission line widths, which enables unbiased measurements even for lines coarsely resolved by narrow-band data. We assess the performance of this technique using quasars from the Sloan Digital Sky Survey (SDSS) observed by the miniJPAS survey, a proof-of-concept project of the Javalambre Physics of the Accelerating Universe Astrophysical Survey (J-PAS) collaboration covering ≃1 deg2 of the northern sky using the 56 J-PAS narrow-band filters. Results. We find remarkable agreement between black hole masses from single-epoch SDSS spectra and single-epoch miniJPAS photometry, with no systematic difference between these and a scatter ranging from 0.4 to 0.07 dex for masses from log(MBH)≃8 to 9.75, respectively. Reverberation mapping studies show that single-epoch masses present approximately 0.4 dex precision, letting us conclude that our novel technique delivers black hole masses with only mildly lower precision than single-epoch spectroscopy. Conclusions. The J-PAS survey will soon start observing thousands of square degrees without any source preselection other than the photometric depth in the detection band, and thus single-epoch photometry has the potential to provide details on the physical properties of quasar populations that do not satisfy the preselection criteria of previous spectroscopic surveys.

show abstract

The stellar host in star-forming low-mass galaxies: Evidence for two classes

Cited by 3 publications

References 89 publications

Multiwavelength Bulge–Disk Decomposition for the Galaxy M81 (NGC 3031). I. Morphology

Multiwavelength Bulge–Disk Decomposition for the Galaxy M81 (NGC 3031). I. Morphology

The miniJPAS survey: Identification and characterization of the emission line galaxies down toz< 0.35 in the AEGIS field

Black hole virial masses from single-epoch photometry

Contact Info

Product

Resources

About