The Manga Integral Field Unit Fiber Feed System for the Sloan 2.5 M Telescope

Drory, Niv; MacDonald, Nicholas; Bershady, M. A.; Bundy, Kevin; Gunn, James E.; Law, David R.; Smith, Michael P.; Stoll, Robert D.; Tremonti, Christy; Wake, David A.; Yan, Renbin; Weijmans, Anne-Marie; Byler, Nell; Cherinka, Brian; Cope, Frances; Eigenbrot, Arthur; Harding, Paul; Holder, Diana; Huehnerhoff, Joseph; Jaehnig, Kurt P.; Jansen, Tiffany; Klaene, Mark A.; Paat, Anthony; Percival, J. W.; Sayres, Conor

doi:10.1088/0004-6256/149/2/77

Cited by 487 publications

(382 citation statements)

References 14 publications

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“…The MaNGA hardware design is described in detail by Drory et al (2015); here we provide a brief summary of the major elements that most closely pertain to the DRP. MaNGA uses the BOSS optical fiber spectrographs (Smee et al 2013) installed on the Sloan Digital Sky Survey 2.5 m telescope (Gunn et al 2006) at Apache Point Observatory (APO) in New Mexico.…”

Section: Hardwarementioning

confidence: 99%

“…These fibers are grouped into four physical blocks on the spectrograph entrance slit (schematic diagram at bottom), with the sky fibers located at the ends of each block. Note that the orientation of this figure is flipped in relation to Figure9 of Drory et al (2015) as the view presented here is on-sky (north up, east left). improvements in cosmic-ray rejection routines and data-qualityassessment statistics.…”

Section: Data Reduction Pipelinementioning

confidence: 99%

“…The DRP automatically assesses the level of scattered light in the MaNGA data by taking advantage of the hardware design in which gaps of ∼16 pixels were left between each v-groove block (compared to ∼4 pixels peak-to-peak between each fiber trace within a block) so that the interstitial regions contain negligible light from the Gaussian fiber profile cores (Drory et al 2015). By masking out everything within five pixels of the fiber traces we can identify those pixels on the edge of the detector and in empty regions between individual blocks whose counts are dominated by diffuse light on the detector.…”

Section: Scattered Lightmentioning

confidence: 99%

“…The individual MaNGA fibers typically have high throughput (see discussion by Drory et al 2015) within 5%-10% of each other. The relative distribution of throughputs is monitored daily to trigger cleaning of the IFU surfaces when the DRP detects noticeable degradation in uniformity or overall throughput.…”

Section: Fiber Flat-fieldmentioning

confidence: 99%

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

Law¹,

Cherinka²,

Yan³

et al. 2016

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444

307

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Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) is an optical fiber-bundle integral-field unit (IFU) spectroscopic survey that is one of three core programs in the fourth-generation Sloan Digital Sky Survey (SDSS-IV). With a spectral coverage of 3622-10354 Å and an average footprint of ∼500 arcsec 2 per IFU the scientific data products derived from MaNGA will permit exploration of the internal structure of a statistically large sample of 10,000 low-redshift galaxies in unprecedented detail. Comprising 174 individually pluggable science and calibration IFUs with a near-constant data stream, MaNGA is expected to obtain ∼100 million raw-frame spectra and ∼10 million reduced galaxy spectra over the six-year lifetime of the survey. In this contribution, we describe the MaNGA Data Reduction Pipeline algorithms and centralized metadata framework that produce skysubtracted spectrophotometrically calibrated spectra and rectified three-dimensional data cubes that combine individual dithered observations. For the 1390 galaxy data cubes released in Summer 2016 as part of SDSS-IV Data Release 13, we demonstrate that the MaNGA data have nearly Poisson-limited sky subtraction shortward of ∼8500 Å and reach a typical 10σ limiting continuum surface brightness μ=23.5 AB arcsec −2 in a five-arcseconddiameter aperture in the g-band. The wavelength calibration of the MaNGA data is accurate to 5 km s −1 rms, with a median spatial resolution of 2.54 arcsec FWHM (1.8 kpc at the median redshift of 0.037) and a median spectral resolution of σ=72 km s −1 .

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Section: Hardwarementioning

confidence: 99%

Section: Data Reduction Pipelinementioning

confidence: 99%

Section: Scattered Lightmentioning

confidence: 99%

Section: Fiber Flat-fieldmentioning

confidence: 99%

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

Law¹,

Cherinka²,

Yan³

et al. 2016

Self Cite

444

307

View full text Add to dashboard Cite

show abstract

“…MaNGA makes use of a modification of the BOSS spectrographs (Smee et al 2013) to bundle fibers into hexagons (Drory et al 2015). Each spectra has a wavelength coverage of 3500-10,000 Å, and instrumental resolution ∼60 km s −1 .…”

Section: Manga Targetsmentioning

confidence: 99%

SDSS-IV MaNGA-resolved Star Formation and Molecular Gas Properties of Green Valley Galaxies: A First Look with ALMA and MaNGA

Lin

Belfiore

Pan

et al. 2017

ApJ

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We study the role of cold gas in quenching star formation in the green valley by analyzing ALMA 12 CO (1-0) observations of three galaxies with resolved optical spectroscopy from the MaNGA survey. We present resolution-matched maps of the star formation rate and molecular gas mass. These data are used to calculate the star formation efficiency (SFE) and gas fraction ( f gas ) for these galaxies separately in the central "bulge" regions and outer disks. We find that, for the two galaxies whose global specific star formation rate (sSFR) deviates most from the star formation main sequence, the gas fraction in the bulges is significantly lower than that in their disks, supporting an "inside-out" model of galaxy quenching. For the two galaxies where SFE can be reliably determined in the central regions, the bulges and disks share similar SFEs. This suggests that a decline in f gas is the main driver of lowered sSFR in bulges compared to disks in green valley galaxies. Within the disks, there exist common correlations between the sSFR and SFE and between sSFR and f gas on kiloparsec scales-the local SFE or f gas in the disks declines with local sSFR. Our results support a picture in which the sSFR in bulges is primarily controlled by f gas , whereas both SFE and f gas play a role in lowering the sSFR in disks. A larger sample is required to confirm if the trend established in this work is representative of the green valley as a whole.

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The Fibre Resolved OpticAl and Near-Ultraviolet Czerny–Turner Imaging Spectropolarimeter (francis)

Jess,

Grant,

Bate

et al. 2023

Sol Phys

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The solar physics community is entering a golden era that is ripe with next-generation ground- and space-based facilities, advanced spectral inversion techniques, and realistic simulations that are becoming more computationally streamlined and efficient. With ever-increasing resolving power stemming from the newest observational telescopes, it becomes more challenging to obtain (near-)simultaneous measurements at high spatial, temporal and spectral resolutions, while operating at the diffraction limit of these new facilities. Hence, in recent years there has been increased interest in the capabilities integral field units (IFUs) offer towards obtaining the trifecta of high spatial, temporal and spectral resolutions contemporaneously. To date, IFUs developed for solar physics research have focused on mid-optical and infrared measurements. Here, we present an IFU prototype that has been designed for operation within the near-ultraviolet to mid-optical wavelength range, which enables key spectral lines (e.g., Ca ii H/K, H$\beta $ β , Sr ii, Na i D1/D2, etc.) to be studied, hence providing additional spectral coverage to the instrument suites developed to date. The IFU was constructed as a low-budget proof-of-concept for the upcoming $2\text{ m}$ 2 m class Indian National Large Solar Telescope and employs circular cross-section fibres to guide light into a Czerny–Turner configuration spectrograph, with the resulting spectra captured using a high quantum efficiency scientific CMOS camera. Mapping of each input fibre allows for the reconstruction of two-dimensional spectral images, with frame rates exceeding $20\text{ s}^{-1}$ 20 s − 1 possible while operating in a non-polarimetric configuration. Initial commissioning of the instrument was performed at the Dunn Solar Telescope, USA, during August 2022. The science verification data presented here highlights the suitability of fibre-fed IFUs operating at near-ultraviolet wavelengths for solar physics research. Importantly, the successful demonstration of this type of instrument paves the way for further technological developments to make a future variant suitable for upcoming ground-based and space-borne telescope facilities.

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The Manga Integral Field Unit Fiber Feed System for the Sloan 2.5 M Telescope

Cited by 487 publications

References 14 publications

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

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

SDSS-IV MaNGA-resolved Star Formation and Molecular Gas Properties of Green Valley Galaxies: A First Look with ALMA and MaNGA

The Fibre Resolved OpticAl and Near-Ultraviolet Czerny–Turner Imaging Spectropolarimeter (francis)

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