THE DATA REDUCTION PIPELINE FOR THE SDSS-IV MaNGA IFU GALAXY SURVEY

Law, David R.; Cherinka, Brian; Yan, Renbin; Andrews, Brett H.; Bershady, Matthew A.; Bizyaev, Dmitry; Blanc, Guillermo A.; Blanton, Michael R.; Bolton, A.; Brownstein, Joel R.; Bundy, Kevin; Chen, Yanmei; Drory, Niv; D’Souza, Richard; Fu, Hai; Jones, Amy; Kauffmann, Guinevere; MacDonald, Nicholas; Masters, Karen L.; Newman, Jeffrey A.; Parejko, John K.; Sánchez-Gallego, José R.; Sánchez, S. F.; Schlegel, David J.; Thomas, Daniel; Wake, David A.; Weijmans, Anne-Marie; Westfall, Kyle B.; Zhang, Kai

doi:10.3847/0004-6256/152/4/83

Cited by 427 publications

(317 citation statements)

References 74 publications

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“…We processed our data using version 2_2_0 of the MaNGA Data Reduction Pipeline (DRP; Law et al 2015Law et al , 2016. This version is similar to v2_1_2 released in 2017 July as SDSS DR14 (Abolfathi et al 2018), but incorporates a number of custom modifications made specifically for the Deep Coma program.…”

Section: Data Reductionmentioning

confidence: 99%

Low Metallicities and Old Ages for Three Ultra-diffuse Galaxies in the Coma Cluster

Conroy

Law

et al. 2018

ApJ

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A large population of ultra-diffuse galaxies (UDGs) was recently discovered in the Coma cluster. Here we present optical spectra of three such UDGs, DF7, DF44, and DF17, which have central surface brightnesses of μ g ≈24.4-25.1 mag arcsec −2 . The spectra were acquired as part of an ancillary program within the SDSS-IV MaNGA Survey. We stacked 19 fibers in the central regions from larger integral field units (IFUs) per source. With over 13.5 hr of on-source integration, we achieved a mean signal-to-noise ratio in the optical of 9.5 Å −1 , 7.9 Å −1 , and 5.0 Å −1 , respectively, for DF7, DF44, and DF17. Stellar population models applied to these spectra enable measurements of recession velocities, ages, and metallicities. respectively. Their stellar masses are (3-6)×10 8 M e . The UDGs in our sample are as old or older than galaxies at similar stellar mass or velocity dispersion (only DF 44 has an independently measured dispersion). They all follow the well-established stellar mass-stellar metallicity relation, while DF44 lies below the velocity dispersionmetallicity relation. These results, combined with the fact that UDGs are unusually large for their stellar masses, suggest that stellar mass plays a more important role in setting stellar population properties for these galaxies than either size or surface brightness.

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Section: Data Reductionmentioning

confidence: 99%

Low Metallicities and Old Ages for Three Ultra-diffuse Galaxies in the Coma Cluster

Conroy

Law

et al. 2018

ApJ

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“…Careful spectrophotometry yields a relative calibration accurate to a few percent (Yan et al 2016b). The survey design is described in Yan et al (2016a), the observing strategy in Law et al (2015), and the data reduction pipeline in Law et al (2016). The MaNGA team has also developed useful tools for data visualization and vetting (Cherinka et al 2017).…”

Section: The Manga Surveymentioning

confidence: 99%

“…The resolution as a function of wavelength is calculated from arcs taken before and after each exposure and then corrected using strong sky lines (Law et al 2016). Tests indicate that these corrections are better than 5% for dispersions of 70 et al 2017, in preparation).…”

Section: Kinematic Measurementsmentioning

confidence: 99%

SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies

Greene

Leauthaud

Emsellem

et al. 2018

ApJ

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We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et al. group catalog, we identify central and satellite galaxies in groups with halo masses in the range . As in previous work, we see a sharp dependence on stellar mass, in the sense that ∼70% of galaxies with stellar mass * > - M h M 10 11 2 tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The ∼30% of high-mass galaxies that have significant rotation do not stand out in other galaxy properties, except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20% level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of central and satellite galaxies with group finders systematically lower differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group-finding methods will have to be forward-modeled via mock catalogs.

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“…On the other hand, the reconstructed PSF of the MaNGA data has an FWHM of ∼2. 5 (Law et al 2016), which corresponds to a physical size of ∼ 1.5 kpc at the mean redshift of the MaNGA survey (Bundy et al 2015). Therefore, although the stars/dust geometry of star-forming regions has a large diversity on small physical scales (Liu et al 2013), the adopted assumption in this work is plausible for our sample.…”

Section: Effect Of Stars/dust Geometrymentioning

confidence: 85%

“…The FWHM of the reconstructed point spread function (PSF) of the data cubes is about 2. 5 (Law et al 2016). In this work, we take the MaNGA data from the SDSS DR14 2 (Abolfathi et al 2018) as the parent sample, which provides 2812 data cubes.…”

Section: Manga Overviewmentioning

confidence: 99%

Dust Attenuation Curve for Local Subgalactic Star-forming Regions

Teklu

Lin

Kong

et al. 2020

ApJ

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We compile a sample of about 157,000 spaxels from the Mapping Nearby Galaxies at the Apache Point Observatory (MaNGA) survey to derive the average dust attenuation curve for subgalactic star-forming regions of local star-forming galaxies (SFGs) in the optical wavelength, following the method of Calzetti et al. We obtain a D n (4000)-independent average attenuation curve for spaxels with 1.1 ≤ D n (4000) < 1.3, which is similar to the one derived from either local starbursts or normal SFGs. We examine whether and how the shape of the average attenuation curve changes with several local and global physical properties. For spaxels with 1.2 ≤ D n (4000) < 1.3, we find no dependence on either local or global physical properties for the shape of the average attenuation curve. However, for spaxels with younger stellar population (1.1 ≤ D n (4000) < 1.2), shallower average attenuation curves are found for star-forming regions with smaller stellar mass surface density, smaller star formation rate surface density, or those residing in the outer region of galaxies. These results emphasize the risk of using one single attenuation curve to correct the dust reddening for all type of star-forming regions, especially for those with fairly young stellar population.

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THE DATA REDUCTION PIPELINE FOR THE SDSS-IV MaNGA IFU GALAXY SURVEY

Cited by 427 publications

References 74 publications

Low Metallicities and Old Ages for Three Ultra-diffuse Galaxies in the Coma Cluster

Low Metallicities and Old Ages for Three Ultra-diffuse Galaxies in the Coma Cluster

SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies

Dust Attenuation Curve for Local Subgalactic Star-forming Regions

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