AstroSat/UVIT Cluster Photometry in the Northern Disk of M31

Leahy, D. A.; Buick, Megan; Leahy, Cameron

doi:10.3847/1538-3881/ac9058

Cited by 6 publications

(4 citation statements)

References 28 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In order to understand the structure of M31, we investigate how the fitted SED parameters vary over its disk. Using an inclination angle of 77° (Leahy et al 2022a), we calculated the deprojected M31 galactocentric distance of the center of each region (calculated as the average position of all pixels in a region) from the center of M31. At the distance of M31 (785 kpc), 1′ spans 228 pc.…”

Section: Nebular Dust and Star Formation Parameters For The Regions C...mentioning

confidence: 99%

Far-ultraviolet to Far-infrared Spectral Energy Distribution Modeling of the Star Formation History across M31

Leahy,

Hansen,

Hopkins

2024

Self Cite

View full text Add to dashboard Cite

Our neighboring galaxy M31 has been recently surveyed at the far- and near-ultraviolet (FUV and NUV) with the UVIT telescope on AstroSat, which provides unprecedented sensitivity to young stellar populations. Here the UVIT data are supplemented with optical data, near-infrared (IR) data (Spitzer), and mid- and far-IR data (Herschel). The observations are processed to obtain the spectral energy distributions (SEDs) for 73 regions covering M31. The SEDs are modeled using the Cigale SED fitting code with old and young stellar populations. The old stellar population has an age of 12 Gyr across M31 but has longer formation times at further distances from the center. Significant dependences on the position of dust extinction, dust emission, and young stellar population properties are found. Across M31, there are regions with a low-age (≲100 Myr) young population and regions with an intermediate-age (∼1 Gyr) young population. The mass in the young population has declined by a factor of ∼10 for ages 800–100 Myr ago but has increased again for ages ≲100 Myr. This indicates that cold gas available for star formation has been changing over the past Gyr, whether it is caused by a changing merger rate, changing gas infall, or changes in the gas reservoir in M31. We find that the dust luminosity, based on far-IR observations, is driven by the youngest stars, which are primarily measured in the FUV and NUV bands.

show abstract

Section: Nebular Dust and Star Formation Parameters For The Regions C...mentioning

confidence: 99%

Far-ultraviolet to Far-infrared Spectral Energy Distribution Modeling of the Star Formation History across M31

Leahy,

Hansen,

Hopkins

2024

Self Cite

View full text Add to dashboard Cite

show abstract

“…For the innermost 120 arcsec, a very young (25 Myr) metal-poor ([Z/H]~−0.7) population was found. For the disk of M31 [36], 239 clusters in the northeast disk and bulge were modeled to measure ages, masses, metallicities, and extinctions. Cluster measurements are generally more sensitive to young populations than total light because the total light is diluted by the older field stars.…”

Section: Star Formation History Of M31mentioning

confidence: 99%

The Andromeda Galaxy and Its Star Formation History

Leahy

2023

Universe

Self Cite

View full text Add to dashboard Cite

The state of knowledge of the properties of the Andromeda Galaxy (also known as M31) is reviewed. The spatial structure of the Andromeda Galaxy, its main source populations, and the properties of its gas and dust are discussed. To understand the formation history of the Andromeda Galaxy, the critical issues of its star formation history and the gas streams and dwarf galaxies in its surrounding environment are reviewed. Emphasis is on recent studies, with important earlier work described in the references provided here. It is important to understand the Andromeda Galaxy because it is the nearest large external galaxy and is close enough for high-resolution studies. This allows the Andromeda Galaxy to be used as a template for understanding more distant and less resolved galaxies in the universe.

show abstract

“…The UV filter set of the AstroSat UVIT instrument consists of one narrowband filter (N279N), three wideband filters (F148W, F154W, and N242W), and five medium-band filters (F169M, F172M, N219M, N245M, and N263M), where the filter names follow the Hubble Space Telescope (HST) convention that the three digit number represents the central wavelength in nanometers. These filters capture photospheric emission from stellar populations with transmission curves, as shown in Figure 1 ( Leahy et al 2022aLeahy et al , 2022b. The data from AstroSat UVIT can be utilized to discern and model both the age and mass of young stellar populations, ranging from approximately 5-200 Myr and with masses greater than 10 3−4 M e (e.g., Ujjwal et al 2022).…”

Section: Introductionmentioning

confidence: 99%

The PHANGS-AstroSat Atlas of Nearby Star-forming Galaxies

Hassani,

Rosolowsky,

Koch

et al. 2024

ApJS

View full text Add to dashboard Cite

We present the Physics at High Angular resolution in Nearby GalaxieS (PHANGS)-AstroSat atlas, which contains UV imaging of 31 nearby star-forming galaxies captured by the Ultraviolet Imaging Telescope on the AstroSat satellite. The atlas provides a homogeneous data set of far-UV and near-UV maps of galaxies within a distance of 22 Mpc and a median angular resolution of 1.″4 (corresponding to a physical scale between 25 and 160 pc). After subtracting a uniform UV background and accounting for Milky Way extinction, we compare our estimated flux densities to GALEX observations, finding good agreement. We find candidate extended UV disks around the galaxies NGC 6744 and IC 5332. We present the first statistical measurements of the clumping of the UV emission and compare it to the clumping of molecular gas traced with the Atacama Large Millimeter/submillimeter Array (ALMA). We find that bars and spiral arms exhibit the highest degree of clumping, and the molecular gas is even more clumped than the far-UV (FUV) emission in galaxies. We investigate the variation of the ratio of observed FUV to Hα in different galactic environments and kiloparsec-sized apertures. We report that ∼65% of the variation of the log10(FUV/Hα) can be described through a combination of dust attenuation with star formation history parameters. The PHANGS-AstroSat atlas enhances the multiwavelength coverage of our sample, offering a detailed perspective on star formation. When integrated with PHANGS data sets from ALMA, the Very Large Telescope-MUSE, the Hubble Space Telescope, and JWST, it develops our comprehensive understanding of attenuation curves and dust attenuation in star-forming galaxies.

show abstract

AstroSat/UVIT Cluster Photometry in the Northern Disk of M31

Cited by 6 publications

References 28 publications

Far-ultraviolet to Far-infrared Spectral Energy Distribution Modeling of the Star Formation History across M31

Far-ultraviolet to Far-infrared Spectral Energy Distribution Modeling of the Star Formation History across M31

The Andromeda Galaxy and Its Star Formation History

The PHANGS-AstroSat Atlas of Nearby Star-forming Galaxies

Contact Info

Product

Resources

About