Resolved and Integrated Stellar Masses in the SDSS-iv/MaNGA Survey. I. PCA Spectral Fitting and Stellar Mass-to-light Ratio Estimates

Pace, Zachary J.; Tremonti, Christy; Chen, Yanmei; Schaefer, Adam L.; Bershady, Matthew A.; Westfall, Kyle B.; Brownstein, Joel R.; Drory, Niv; Boquien, M.; Rowlands, Kate; Andrews, Brett H.; Wake, David A.

doi:10.3847/1538-4357/ab3723

Cited by 13 publications

(11 citation statements)

References 125 publications

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“…The stellar content of a galaxy is therefore a valuable diagnostic for its integrated star formation and chemical enrichment history. For this work, we take the estimates of stellar mass per spaxel provided by Pace et al (2019aPace et al ( , 2019b. With this method, individual spectra are fitted using a basis set of six vectors, found using principal Figure 1.…”

Section: Stellar Mass Surface Densitymentioning

confidence: 99%

“…Dust attenuation is taken into account using a two-component model following Charlot & Fall (2000), whereby light from the younger component of the stellar population experiences a different degree of extinction than the light from the older stellar populations. Pace et al (2019a) showed that this technique provides statistically robust estimates of the stellar mass-tolight ratio across a wide range of S/Ns, star formation histories, and metallicities, with random uncertainties typically 0.1 dex or less for spectra with S/N>2.…”

Section: Stellar Mass Surface Densitymentioning

confidence: 99%

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SDSS-IV MaNGA: Evidence for Enriched Accretion onto Satellite Galaxies in Dense Environments

Schaefer

Tremonti

Pace

et al. 2019

ApJ

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We investigate the environmental dependence of the local gas-phase metallicity in a sample of star-forming galaxies from the MaNGA survey. Satellite galaxies with stellar masses in the range ()  < < M M 9 log 10 * are found to be ∼0.05 dex higher in metallicity than centrals of similar stellar mass. Within the low-mass satellite population, we find that the interstellar medium (ISM) metallicity depends most strongly on the stellar mass of the galaxy that is central to the halo, though there is no obvious difference in the metallicity gradients. At fixed total stellar mass, the satellites of high-mass (M * > 10 10.5 M e) centrals are ∼0.1 dex more metal-rich than the satellites of low-mass (M * < 10 10 M e) centrals, controlling for local stellar mass surface density and gas fraction. Fitting a gas regulator model to the spaxel data, we are able to account for variations in the local gas fraction, stellar mass surface density, and local escape velocity-dependent outflows. We find that the best explanation for the metallicity differences is the variation in the average metallicity of accreted gas between different environments that depends on the stellar mass of the dominant galaxies in each halo. This is interpreted as evidence for the exchange of enriched gas between galaxies in dense environments that is predicted by recent simulations.

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Section: Stellar Mass Surface Densitymentioning

confidence: 99%

Section: Stellar Mass Surface Densitymentioning

confidence: 99%

SDSS-IV MaNGA: Evidence for Enriched Accretion onto Satellite Galaxies in Dense Environments

Schaefer

Tremonti

Pace

et al. 2019

ApJ

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“…In recent years, full spectral fitting of integrated light spectra to model spectra has opened a new window to study in detail the physical, chemical and evolutionary phases of galaxy stellar populations (e.g. Pérez et al 2013;Pace et al 2019;Boardman et al 2020). Some of the most widely used spectral fitting software for this technique are FIREFLY (Wilkinson et al 2017), STECKMAP (Ocvirk et al 2006), VESPA (Tojeiro 2007), pPXF (Cappellari et al 2009), ULySS (Koleva et al 2009), STARLIGHT (Cid Fernandes et al 2011), andPipe3D (Sánchez et al 2016a,b).…”

Section: Introductionmentioning

confidence: 99%

The APOGEE Library of Infrared SSP Templates (A-LIST): High-resolution Simple Stellar Population Spectral Models in the H Band

Ashok

Zasowski

Seth

et al. 2021

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Integrated light spectroscopy from galaxies can be used to study the stellar populations that cannot be resolved into individual stars. This analysis relies on stellar population synthesis (SPS) techniques to study the formation history and structure of galaxies. However, the spectral templates available for SPS are limited, especially in the near-infrared (near-IR). We present A-LIST (APOGEE Library of Infrared SSP Templates), a new set of high-resolution, near-IR SSP spectral templates spanning a wide range of ages (2–12 Gyr), metallicities ( − 2.2 < [M/H] < + 0.4) and α abundances ( − 0.2 < [α/M] < + 0.4). This set of SSP templates is the highest resolution (R ∼ 22, 500) available in the near-IR, and the first such based on an empirical stellar library. Our models are generated using spectra of ∼300,000 stars spread across the Milky Way, with a wide range of metallicities and abundances, from the APOGEE survey. We show that our model spectra provide accurate fits to M31 globular cluster spectra taken with APOGEE, with best-fit metallicities agreeing with those of previous estimates to within ∼0.1 dex. We also compare these model spectra to lower-resolution E-MILES models and demonstrate that we recover the ages of these models to within ∼1.5 Gyr. This library is available in https://github.com/aishashok/ALIST-library.

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“…This means that the complicated spectral features including more than 30 lines are controlled by several bases represented by the PCs. This advantage itself is a well-known benefit to use the PCA in general as a dimensionality reduction method (e.g., Galaz & de Lapparent 1998;Ronen et al 1999;Wang et al 2011;Pace et al 2019;Portillo et al 2020, among many others), but all these previous applications were on integrated 1-d spectra with sufficiently large number of n, namely, not HDLSS data. We stress that the analysis in this work is substantially different from these works: the current method is able to be applied to a spectral map which is a typical HDLSS dataset and traditional PCA would not have worked due to the huge noise sphere, as mentioned in Section 2.…”

Section: Distribution Of the Contribution Of Pcsmentioning

confidence: 99%

High Dimensional Statistical Analysis and its Application to ALMA Map of NGC 253

Takeuchi¹,

Yata²,

Aoshima³

et al. 2022

Preprint

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In astronomy, if we denote the dimension of data as d and the number of samples as n, we often meet a case with n d. Traditionally, such a situation is regarded as ill-posed, and there was no choice but to throw away most of the information in data dimension to let d < n. The data with n d is referred to as high-dimensional low sample size (HDLSS). To deal with HDLSS problems, a method called high-dimensional statistics has been developed rapidly in the last decade. In this work, we first introduce the high-dimensional statistical analysis to the astronomical community. We apply two representative methods in the high-dimensional statistical analysis methods, the noise-reduction principal component analysis (NRPCA) and regularized principal component analysis (RPCA), to a spectroscopic map of a nearby archetype starburst galaxy NGC 253 taken by the Atacama Large Millimeter/Submillimeter Array (ALMA). The ALMA map is a typical HDLSS dataset. First we analyzed the original data including the Doppler shift due to the systemic rotation. The high-dimensional PCA could describe the spatial structure of the rotation precisely. We then applied to the Doppler-shift corrected data to analyze more subtle spectral features. The NRPCA and RPCA could quantify the very complicated characteristics of the ALMA spectra. Particularly, we could extract the information of the global outflow from the center of NGC 253. This method can also be applied not only to spectroscopic survey data, but also any type of data with small sample size and large dimension.

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Resolved and Integrated Stellar Masses in the SDSS-iv/MaNGA Survey. I. PCA Spectral Fitting and Stellar Mass-to-light Ratio Estimates

Cited by 13 publications

References 125 publications

SDSS-IV MaNGA: Evidence for Enriched Accretion onto Satellite Galaxies in Dense Environments

SDSS-IV MaNGA: Evidence for Enriched Accretion onto Satellite Galaxies in Dense Environments

The APOGEE Library of Infrared SSP Templates (A-LIST): High-resolution Simple Stellar Population Spectral Models in the H Band

High Dimensional Statistical Analysis and its Application to ALMA Map of NGC 253

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