Red and Reddened: Ultraviolet through Near-infrared Observations of Type Ia Supernova 2017erp*

Brown, P. J.; Hosseinzadeh, G.; Jha, Saurabh W.; Sand, David J.; Vieira, Ethan; Wang, Xiaofeng; Dai, Mi; Dettman, K.; Mould, Jeremy; Uddin, S. A.; Wang, Lifan; Arcavi, I.; Bento, J.; Burns, C. R.; Diamond, T.; Hiramatsu, D.; Howell, D. A.; Hsiao, E. Y.; Marion, G. H.; McCully, C.; Milne, Peter; Mirzaqulov, D. O.; Ruiter, Ashley J.; Valenti, S.; Xiang, Danfeng

doi:10.3847/1538-4357/ab1a3f

Cited by 30 publications

(19 citation statements)

References 103 publications

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“…The new SBF distances are also part of a concurrent study by Milne et al (2021) that explores the dependence of SN luminosity on galaxy type for the "narrow-normal" SN Ia population. These SBF distances are crucial to extending the SN distance calibration to ETGs for which Cepheid distances are not available, and for determining the relationship between SN luminosity and UV color (Milne et al 2013(Milne et al , 2015Brown et al 2017Brown et al , 2019.…”

Section: Supernova Luminosity Calibrationmentioning

confidence: 99%

Infrared Surface Brightness Fluctuation Distances for MASSIVE and Type Ia Supernova Host Galaxies*

Jensen

Blakeslee

et al. 2021

ApJS

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We measured high-quality surface brightness fluctuation (SBF) distances for a sample of 63 massive early-type galaxies using the WFC3/IR camera on the Hubble Space Telescope. The median uncertainty on the SBF distance measurements is 0.085 mag, or 3.9% in distance. Achieving this precision at distances of 50–100 Mpc required significant improvements to the SBF calibration and data analysis procedures for WFC3/IR data. Forty-two of the galaxies are from the MASSIVE Galaxy Survey, a complete sample of massive galaxies within ∼100 Mpc; the SBF distances for these will be used to improve the estimates of the stellar and central supermassive black hole masses in these galaxies. Twenty-four of the galaxies are Type Ia supernova hosts, useful for calibrating SN Ia distances for early-type galaxies and exploring possible systematic trends in the peak luminosities. Our results demonstrate that the SBF method is a powerful and versatile technique for measuring distances to galaxies with evolved stellar populations out to 100 Mpc and constraining the local value of the Hubble constant.

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Section: Supernova Luminosity Calibrationmentioning

confidence: 99%

Infrared Surface Brightness Fluctuation Distances for MASSIVE and Type Ia Supernova Host Galaxies*

Jensen

Blakeslee

et al. 2021

ApJS

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“…The parameters of these six new SNe Ia are given in Table 3. (7) This work, using the method given by Zheng et al (2017b), (8) This paper, (9) Brown et al (2019). Reddening values are given in mag.…”

Section: Early-time Color Evolutionmentioning

confidence: 99%

SN 2017cfd: A Normal Type Ia Supernova Discovered Very Young

Han

Zheng

Stahl

et al. 2020

ApJ

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The Type Ia supernova (SN Ia) 2017cfd in IC 0511 (redshift z = 0.01209 ± 0.00016) was discovered by the Lick Observatory Supernova Search 1.6 ± 0.7 d after the fitted first-light time (FFLT; 15.2 d before B-band maximum brightness). Photometric and spectroscopic follow-up observations show that SN 2017cfd is a typical, normal SN Ia with a peak luminosity M B ≈ −19.2±0.2 mag, ∆m 15 (B) = 1.16 mag, and reached a B-band maximum ∼16.8 d after the FFLT. We estimate there to be moderately strong host-galaxy extinction (A V = 0.39 ± 0.03 mag) based on MLCS2k2 fitting. The spectrum reveals a Si II λ6355 velocity of ∼ 11, 200 km s −1 at peak brightness. SN 2017cfd was discovered very young, with multiband data taken starting 2 d after the FFLT, making it a valuable complement to the currently small sample (fewer than a dozen) of SNe Ia with color data at such early times. We find that its intrinsic early-time (B − V ) 0 color evolution belongs to the "blue" population rather than to the distinct "red" population. Using the photometry, we constrain the companion star radius to be 2.5 R , thus ruling out a red-giant companion.

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“…Regardless of whether the NUV-blue/red groups are distinct or a continuous color parameter, they are not related to the host galaxy metallicity. This seems to contradict the conclusions of Brown et al (2019) if the metallicity differences of the Walker et al (2012) models are attributed to the progenitor metallicity. Recent measurements of the gas phase metallicity in two star forming regions in NGC 5861 point to a subsolar metallicity (12 + log(OH)=7.67 ± 0.01 and 7.87 ± 0.03; Muñoz-Vergara et al 2019) for the host of the NUV-red SN 2017erp.…”

Section: Discussionmentioning

confidence: 80%

“…Brown et al (2015) also showed, however, that the UV flux levels of the Lentz et al (2000) models were too high and that even the relative color differences between objects did not match the multi-epoch color differences of SNe 2011by and 2011fe. Using a different set of models from Walker et al (2012), Brown et al (2019) found that SN 2011fe had UV flux levels comparable to lowmetallicity models while the redder SN 2017erp featured a depressed UV continuum which matched the highermetallicity models. From the observations, it is clear that significant but distinct variations appear in the mid-UV and near-UV wavelength regions; however, the same physical difference -metallicity -has been invoked for both of the spectral ranges.…”

Section: Introductionmentioning

confidence: 96%

A Photometric Analysis of the Relationship between the UV flux of Type Ia Supernovae and Host-galaxy Metallicity

Brown

Crumpler

2020

ApJ

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The effect of progenitor metallicity on Type Ia Supernovae (SNe Ia) has important cosmological implications due to the need for these standardizable candles to be compared across large spans of cosmic time in which the progenitor stars might have different properties. Theoretical models have come to different conclusions as to the wavelength range impacted by metallicity differences, leading to differing interpretations of the growing sample of UV observations. Recent work has claimed a correlation between the mid-UV flux of SNe Ia measured from Swift grism spectra and the gas-phase metallicities measured for their host galaxies. Here we examine UV photometry for the same objects. We find no significant correlations between the UV-optical colors (or UV/optical count rate ratios) of the SNe Ia and the host galaxy properties of mass or metallicity. The lack of a significant correlation with host galaxy metallicity implies another physical difference other than progenitor metallicity dominates the UV flux differences. We are no longer limited by a lack of UV observations. Rather, understanding the existing observations requires improved theoretical models and a larger parameter space of physical differences.

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Red and Reddened: Ultraviolet through Near-infrared Observations of Type Ia Supernova 2017erp*

Cited by 30 publications

References 103 publications

Infrared Surface Brightness Fluctuation Distances for MASSIVE and Type Ia Supernova Host Galaxies*

Infrared Surface Brightness Fluctuation Distances for MASSIVE and Type Ia Supernova Host Galaxies*

SN 2017cfd: A Normal Type Ia Supernova Discovered Very Young

A Photometric Analysis of the Relationship between the UV flux of Type Ia Supernovae and Host-galaxy Metallicity

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