PypeIt: The Python Spectroscopic Data Reduction Pipeline

Prochaska, J. Xavier; Hennawi, Joseph F.; Westfall, Kyle B.; Cooke, Ryan; Wang, Feige; Hsyu, Tiffany; Davies, Frederick B.; Farina, Emanuele Paolo; Pelliccia, Debora

doi:10.21105/joss.02308

Cited by 243 publications

(146 citation statements)

References 12 publications

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“…All optical and NIR spectroscopic data were reduced by applying standard data reduction techniques with the newly developed open source Python spectroscopic data reduction package PypeIt (Prochaska et al 2020a(Prochaska et al , 2020b. The reduction procedure includes sky subtraction, which was performed on the 2D images by including both image differencing between dithered exposures (whenever these were available) and a B-spline fitting procedure.…”

Section: Keck/deimos Observationsmentioning

confidence: 99%

Detecting and Characterizing Young Quasars. I. Systemic Redshifts and Proximity Zone Measurements

Eilers

Hennawi

Decarli³

et al. 2020

ApJ

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In a multiwavelength survey of 13 quasars at 5.8z6.5, which were preselected to be potentially young, we find five objects with extremely small proximity zone sizes that may imply UV-luminous quasar lifetimes of 100,000 yr. Proximity zones are regions of enhanced transmitted flux in the vicinity of quasars that are sensitive to the quasars' lifetimes because the intergalactic gas has a finite response time to their radiation. We combine submillimeter observations from the Atacama Large Millimetre Array and the NOrthern Extended Millimeter Array, as well as deep optical and near-infrared spectra from the medium-resolution spectrograph on the Very Large Telescope and on the Keck telescopes, in order to identify and characterize these new young quasars, which provide valuable clues about the accretion behavior of supermassive black holes in the early universe and pose challenges on current black hole formation models to explain the rapid formation of billion-solar-mass black holes. We measure the quasars' systemic redshifts, black hole masses, Eddington ratios, emission-line luminosities, and star formation rates of their host galaxies. Combined with previous results, we estimate the fraction of young objects within the high-redshift quasar population at large to be 5%f young 10%. One of the young objects, PSO J158-14, shows a very bright dust continuum flux (F cont =3.46±0.02 mJy), indicating a highly starbursting host galaxy with a star formation rate of approximately 1420 M e yr −1 .

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Section: Keck/deimos Observationsmentioning

confidence: 99%

Detecting and Characterizing Young Quasars. I. Systemic Redshifts and Proximity Zone Measurements

Eilers

Hennawi

Decarli³

et al. 2020

ApJ

Self Cite

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“…We also observed the flux standard star Feige 110. We reduced the NIRES data using a newly developed opensource Python-based spectroscopic data reduction pipeline (PypeIt 15 ; Prochaska et al 2019;Prochaska et al 2020). Basic image processing (i.e., flat-fielding) followed standard techniques.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…Software: astropy (Astropy Collaboration et al 2013), emcee (Foreman-Mackey et al 2013), matplotlib (Hunter 2007), PypeIt (Prochaska et al 2019). Fabian Walter https://orcid.org/0000-0003-4793-7880 Minghao Yue https://orcid.org/0000-0002-5367-8021…”

Section: Orcid Idsmentioning

confidence: 99%

A Significantly Neutral Intergalactic Medium Around the Luminous z = 7 Quasar J0252–0503

Wang

Davies

Yang

et al. 2020

ApJ

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158

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Luminous z7 quasars provide direct probes of the evolution of supermassive black holes (SMBHs) and the intergalactic medium (IGM) during the epoch of reionization (EoR). The Lyα damping wing absorption imprinted by neutral hydrogen in the IGM can be detected in a single EoR quasar spectrum, allowing the measurement of the IGM neutral fraction toward that line of sight. However, damping wing features have only been detected in two z>7 quasars in previous studies. In this paper, we present new high-quality optical and near-infrared 3 Q 8. This is the highest IGM neutral fraction yet measured using reionization-era quasar spectra.

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“…SEDM spectra were reduced using the pipeline described by Rigault et al (2019), and the spectra from La Palma were reduced using standard pipelines and procedures for each telescope and instrument. The ALFOSC spectra were often reduced using PypeIt (Prochaska et al 2020). All spectral data and corresponding information is available via WISeREP 15 (Yaron & Gal-Yam 2012).…”

Section: Optical Spectroscopymentioning

confidence: 99%

The Type II supernova SN 2020jfo in M 61, implications for progenitor system, and explosion dynamics

Sollerman

Yang

Schulze

et al. 2021

A&A

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We present the discovery and extensive follow-up observations of SN 2020jfo, a Type IIP supernova (SN) in the nearby (14.5 Mpc) galaxy M 61. Optical light curves (LCs) and spectra from the Zwicky Transient Facility (ZTF), complemented with data from Swift/UVOT and near-infrared photometry is presented. These were used to model the 350-day duration bolometric light curve, which exhibits a relatively short (∼65 days) plateau. This implies a moderate ejecta mass (∼5 M⊙) at the time of explosion, whereas the deduced amount of ejected radioactive nickel is ∼0.025 M⊙. An extensive series of spectroscopy is presented, including spectropolarimetric observations. The nebular spectra are dominated by Hα, but also reveal emission lines from oxygen and calcium. Comparisons to synthetic nebular spectra indicate an initial progenitor mass of ∼12 M⊙. We also note the presence of stable nickel in the nebular spectrum, and SN 2020jfo joins a small group of SNe that have inferred super-solar Ni/Fe ratios. Several years of prediscovery data were examined, but no signs of precursor activity were found. Pre-explosion Hubble Space Telescope imaging reveals a probable progenitor star, detected only in the reddest band (MF814W ≈ −5.8) and it is fainter than expected for stars in the 10−15 M⊙ range. There is thus some tension between the LC analysis, the nebular spectral modeling, and the pre-explosion imaging. To compare and contrast, we present two additional core-collapse SNe monitored by the ZTF, which also have nebular Hα-dominated spectra. This illustrates how the absence or presence of an interaction with circumstellar material (CSM) affect both the LCs and in particular the nebular spectra. Type II SN 2020amv has a LC powered by CSM interaction, in particular after ∼40 days when the LC is bumpy and slowly evolving. The late-time spectra show strong Hα emission with a structure suggesting emission from a thin, dense shell. The evolution of the complex three-horn line profile is reminiscent of that observed for SN 1998S. Finally, SN 2020jfv has a poorly constrained early-time LC, but it is of interest because of the transition from a hydrogen-poor Type IIb to a Type IIn, where the nebular spectrum after the light-curve rebrightening is dominated by Hα, although with an intermediate line width.

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PypeIt: The Python Spectroscopic Data Reduction Pipeline

Cited by 243 publications

References 12 publications

Detecting and Characterizing Young Quasars. I. Systemic Redshifts and Proximity Zone Measurements

Detecting and Characterizing Young Quasars. I. Systemic Redshifts and Proximity Zone Measurements

A Significantly Neutral Intergalactic Medium Around the Luminous z = 7 Quasar J0252–0503

The Type II supernova SN 2020jfo in M 61, implications for progenitor system, and explosion dynamics

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