New Modules for the SEDMachine to Remove Contaminations from Cosmic Rays and Non-target Light: byecr and contsep

Kim, Young-Lo; Rigault, M.; Neill, James D.; Briday, Martin; Copin, Y.; Lezmy, J.; Nicolas, N.; Riddle, Reed; Sharma, Y.; Smith, M.; Sollerman, J.; Walters, Richard

doi:10.1088/1538-3873/ac50a0

Cited by 23 publications

(16 citation statements)

References 31 publications

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“…The light curve, thus far, spans a large phase range from 2021-07-01.4 to 2021-11-11.11 (Figure 3 shows the range used in the fit). We have also obtained a well-sampled spectral time series, beginning with a classification spectrum with the SEDmachine (Blagorodnova et al 2018;Rigault et al 2019;Kim et al 2022) on 2021 July 5. These are presented in detail in a companion paper (L. Harvey et al 2022, in preparation).…”

Section: Methodsmentioning

confidence: 99%

A Uniform Type Ia Supernova Distance Ladder with the Zwicky Transient Facility: Absolute Calibration Based on the Tip of the Red Giant Branch Method

Dhawan

Goobar

Johansson

et al. 2022

ApJ

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The current Cepheid-calibrated distance ladder measurement of H 0 is reported to be in tension with the values inferred from the cosmic microwave background (CMB), assuming standard cosmology. However, some tip of the red giant branch (TRGB) estimates report H 0 in better agreement with the CMB. Hence, it is critical to reduce systematic uncertainties in local measurements to understand the Hubble tension. In this paper, we propose a uniform distance ladder between the second and third rungs, combining Type Ia supernovae (SNe Ia) observed by the Zwicky Transient Facility (ZTF) with a TRGB calibration of their absolute luminosity. A large, volume-limited sample of both calibrator and Hubble flow SNe Ia from the same survey minimizes two of the largest sources of systematics: host-galaxy bias and nonuniform photometric calibration. We present results from a pilot study using the existing TRGB distance to the host galaxy of ZTF SN Ia SN 2021rhu (aka ZTF21abiuvdk) in NGC7814. Combining the ZTF calibrator with a volume-limited sample from the first data release of ZTF Hubble flow SNe Ia, we infer H 0 = 76.94 ± 6.4 km s−1 Mpc−1, an 8.3% measurement. The error budget is dominated by the single object calibrating the SN Ia luminosity in this pilot study. However, the ZTF sample includes already five other SNe Ia within ∼20 Mpc for which TRGB distances can be obtained with the Hubble Space Telescope. Finally, we present the prospects of building this distance ladder out to 80 Mpc with James Webb Space Telescope observations of more than 100 ZTF SNe Ia.

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Section: Methodsmentioning

confidence: 99%

A Uniform Type Ia Supernova Distance Ladder with the Zwicky Transient Facility: Absolute Calibration Based on the Tip of the Red Giant Branch Method

Dhawan

Goobar

Johansson

et al. 2022

ApJ

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“…The SEDM spectra were reduced with PYSEDM 7 (Rigault et al 2019 ;Kim et al 2022 ). All long-slit spectral observations were reduced using standard IRAF/PYRAF 8 and IDL / PYTHON routines for bias subtractions and flat fielding of the two-dimensional spectral images.…”

Section: Spectroscopymentioning

confidence: 99%

SN 2021zny: an early flux excess combined with late-time oxygen emission suggests a double white dwarf merger event

Dimitriadis

Maguire

Karambelkar

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present a photometric and spectroscopic analysis of the ultra-luminous and slowly evolving 03fg-like Type Ia SN 2021zny. Our observational campaign starts from ∼5.3 hours after explosion (making SN 2021zny one of the earliest observed members of its class), with dense multi-wavelength coverage from a variety of ground- and space-based telescopes, and is concluded with a nebular spectrum ∼10 months after peak brightness. SN 2021zny displayed several characteristics of its class, such as the peak brightness (MB = −19.95 mag), the slow decline (Δm15(B) = 0.62 mag), the blue early-time colours, the low ejecta velocities and the presence of significant unburned material above the photosphere. However, a flux excess for the first ∼1.5 days after explosion is observed in four photometric bands, making SN 2021zny the third 03fg-like event with this distinct behavior, while its +313 d spectrum shows prominent [O i] lines, a very unusual characteristic of thermonuclear SNe. The early flux excess can be explained as the outcome of the interaction of the ejecta with ∼0.04 M⊙ of H/He-poor circumstellar material at a distance of ∼1012 cm, while the low ionization state of the late-time spectrum reveals low abundances of stable iron-peak elements. All our observations are in accordance with a progenitor system of two carbon/oxygen white dwarfs that undergo a merger event, with the disrupted white dwarf ejecting carbon-rich circumstellar material prior to the primary white dwarf detonation.

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“…• 1.5 m telescope at Palomar Observatory; 16 epochs. Data were acquired with the integral field unit (IFU) SEDM, and reduced using the automatic SEDM pipeline (Rigault et al 2019;Kim et al 2022).…”

Section: Spectroscopymentioning

confidence: 99%

SN 2022oqm -- a Ca-rich explosion of a compact progenitor embedded in C/O circumstellar material

Irani¹,

Chen²,

Morag³

et al. 2022

Preprint

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We present the discovery and analysis of SN 2022oqm, a Type Ic supernova (SN) detected < 1 day after explosion. The SN rises to a blue and short-lived (2 days) initial peak. Early spectral observations of SN 2022oqm show a hot (40,000 K) continuum with high-ionization C and O absorption features at velocities of 4,000 km s −1 , while its photospheric radius expands at 20,000 km s −1 , indicating a pre-existing distribution of expanding C/O material, likely ejected ∼ 2 weeks before the explosion. After ∼ 2.5 days, both the spectrum and light curves evolve into those of a typical SN Ic, with line velocities of 10, 000 km s −1 , in agreement with the photospheric radius evolution. The optical light curves reach a second peak around t ∼ 15 days. By t = 60 days, the spectrum of SN 2022oqm becomes nearly nebular, displaying strong Ca II and [Ca II] emission with no detectable [O I] and marking this event as Ca-rich. The early behavior can be explained by 10 −3 M of optically thin circumstellar material (CSM) surrounding either (1) a massive compact progenitor such as a Wolf-Rayet star, (2) a massive stripped progenitor with an extended envelope, or (3) a binary system with a white dwarf. We propose that the early-time light curve is powered by a combination of interaction of the ejecta with the optically thin CSM and shock cooling (in the massive-star scenario), until the radioactive decay of 56 Ni becomes the dominant power source. The observations can be explained by CSM that is optically thick to X-ray photons which are down converted, is optically thick in the lines as seen in the spectra, and is optically thin to visible-light continuum photons that come either from down-converted X-rays or from the shock-heated ejecta. Calculations show that this scenario is self-consistent.

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New Modules for the SEDMachine to Remove Contaminations from Cosmic Rays and Non-target Light: byecr and contsep

Cited by 23 publications

References 31 publications

A Uniform Type Ia Supernova Distance Ladder with the Zwicky Transient Facility: Absolute Calibration Based on the Tip of the Red Giant Branch Method

A Uniform Type Ia Supernova Distance Ladder with the Zwicky Transient Facility: Absolute Calibration Based on the Tip of the Red Giant Branch Method

SN 2021zny: an early flux excess combined with late-time oxygen emission suggests a double white dwarf merger event

SN 2022oqm -- a Ca-rich explosion of a compact progenitor embedded in C/O circumstellar material

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