TESSreduce: transient focused TESS data reduction pipeline

Ridden-Harper, Ryan; Rest, A.; Hounsell, R.; Müller-Bravo, T. E.; Wang, Q.; Villar, V. Ashley

doi:10.48550/arxiv.2111.15006

Cited by 7 publications

(7 citation statements)

References 69 publications

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“…Finally, the field of CGCG 438-018 was serendipitously observed by the Transiting Exoplanet Survey Satellite ( TESS ; Ricker et al 2015 ), during Year 4 of the surv e y, at Sector 43, from UT 2021 September 16 until October 12, co v ering the rise up to ∼1 d before peak brightness. TESS data were reduced and calibrated with TESSreduce , 4 a dedicated pipeline optimized for SN photometry (Ridden-Harper et al 2021 ). For additional information on the reduction steps, we refer to Tinyanont et al ( 2022 ).…”

Section: Photometrymentioning

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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Section: Photometrymentioning

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 used the same light-curve extraction method as in Fausnaugh et al (2021), which employs difference imaging and forced photometry with a model of the TESS point-spread function (PSF), using the ISIS software package (Alard & Lupton 1998;Alard 2000). Difference imaging and forced photometry work well for faint sources in TESS images; in addition to ISIS, a pipeline specific to TESS using a similar approach, TESSreduce, was developed by Ridden-Harper et al (2021). The primary challenge for the SN work presented here is the TESS backgrounds.…”

Section: Light Curves and Sn Samplementioning

confidence: 99%

Four Years of Type Ia Supernovae Observed by TESS: Early-time Light-curve Shapes and Constraints on Companion Interaction Models

Fausnaugh,

Vallely,

Tucker

et al. 2023

ApJ

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We present 307 type Ia supernova (SN) light curves from the first 4 yr of the Transiting Exoplanet Survey Satellite mission. We use this sample to characterize the shapes of the early-time light curves, measure the rise times from first light to peak, and search for companion star interactions. Using simulations, we show that light curves must have noise <10% of the peak flux to avoid biases in the early-time light-curve shape, restricting our quantitative analysis to 74 light curves. We find that the mean power-law index t β 1 of the early-time light curves is β 1 = 1.93 ± 0.57, and the mean rise time to peak is 15.7 ± 3.5 days. The underlying population distribution for β 1 may instead consist of a Gaussian component with mean 2.29, width 0.34, and a long tail extending to values less than 1.0. We find that the data can rarely distinguish between models with and without companion interaction models. Nevertheless, we find three high-quality light curves that tentatively prefer the addition of a companion interaction model, but the statistical evidence for the companion interactions is not robust. We also find two SNe that disfavor the addition of a companion interaction model to a curved power-law model. Taking the 74 SNe together, we calculate 3σ upper limits on the presence of companion signatures to control for orientation effects that can hide companions in individual light curves. Our results rule out common progenitor systems with companions having Roche lobe radii >31 R ⊙ (separations >5.7 × 1012 cm, 99.9% confidence level) and disfavor companions having Roche lobe radii >10 R ⊙ (separations >1.9 × 1012 cm, 95% confidence level). Lastly, we discuss the implications of our results for the intrinsic fraction of single degenerate progenitor systems.

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“…32 These three sectors covered preexplosion (S42), double-peaked rise (S43), and decline (S44), which gives excellent coverage of the event outside of the 1 day midsector and inter-sector gaps. We reduced all sectors of TESS data using the TESSreduce python package, which aligns images, subtracts the variable background, and provides a flux calibration from field stars (Ridden-Harper et al 2021). One alteration was made to the default TESSreduce reduction where we included the nearby bad column 1167 in S43 data into the automatically determined strap mask.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Revealing the Progenitor of SN 2021zby through Analysis of the TESS Shock-cooling Light Curve

Wang

Armstrong

Zenati

et al. 2023

ApJL

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We present early observations and analysis of the double-peaked Type IIb supernova (SN IIb) SN 2021zby. TESS captured the prominent early shock-cooling peak of SN 2021zby within the first ∼10 days after explosion with a 30 minute cadence. We present optical and near-infrared spectral series of SN 2021zby, including three spectra during the shock-cooling phase. Using a multiband model fit, we find that the inferred properties of its progenitor are consistent with a red supergiant or yellow supergiant, with an envelope mass of ∼0.30–0.65 M ⊙ and an envelope radius of ∼120–300 R ⊙. These inferred progenitor properties are similar to those of other SNe IIb with a double-peaked feature, such as SNe 1993J, 2011dh, 2016gkg, and 2017jgh. This study further validates the importance of the high cadence and early coverage in resolving the shape of the shock-cooling light curve, while the multiband observations, particularly UV, are also necessary to fully constrain the progenitor properties.

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TESSreduce: transient focused TESS data reduction pipeline

Cited by 7 publications

References 69 publications

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

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

Four Years of Type Ia Supernovae Observed by TESS: Early-time Light-curve Shapes and Constraints on Companion Interaction Models

Revealing the Progenitor of SN 2021zby through Analysis of the TESS Shock-cooling Light Curve

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