TheHubbleHigherzSupernova Search: Supernovae toz≈ 1.6 and Constraints on Type Ia Progenitor Models

Strolger, Louis-Gregory; Riess, Adam G.; Dahlén, T.; Livio, Mario; Panagia, N.; Challis, P.; Tonry, J.; Filippenko, A. V.; Chornock, R.; Ferguson, Henry C.; Koekemoer, Anton M.; Mobasher, Bahram; Dickinson, Mark; Giavalisco, Mauro; Casertano, Stefano; Hook, R. N.; Bondin, Stephane; Leibundgut, B.; Nonino, M.; Rosati, P.; Spinrad, Hyron; Steidel, Charles C.; Stern, Daniel; Garnavich, P.; Matheson, T.; Grogin, Norman A.; Hornschemeier, A. E.; Kretchmer, C.; Laidler, V. G.; Lee, Kyoungsoo; Lucas, Ray A.; Mello, Duília de; Moustakas, Leonidas A.; Ravindranath, Swara; Richardson, Marin; Taylor, Edward N.

doi:10.1086/422901

Cited by 274 publications

(355 citation statements)

References 62 publications

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“…Assuming that φ(t) has a Gaussian shape, they found a preferred delay time of τ ∼ 3-4 Gyr, which is significantly longer than that found when using the specific SNR described above. We note that the main driver of the relatively long delaytime found in the method used by Strolger et al (2004) is the low number of type Ia SNe found at high redshift z > 1.4. Using the extended GOODS survey, Dahlen et al (2008) also found fewer type Ia SNe at z > 1.4 than what is expected if the delaytime is short and SNR follows the SFR.…”

Section: Type Ia Snementioning

confidence: 89%

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Near-IR search for lensed supernovae behind galaxy clusters

Goobar

Paech

Stanishev³

et al. 2009

A&A

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Aims. Powerful gravitational telescopes in the form of massive galaxy clusters can be used to enhance the light collecting power over a limited field of view by about an order of magnitude in flux. This effect is exploited here to increase the depth of a survey for lensed supernovae at near-IR wavelengths. Methods. We present a pilot supernova search programme conducted with the ISAAC camera at VLT. Lensed galaxies behind the massive clusters A1689, A1835, and AC114 were observed for a total of 20 h divided into 2, 3, and 4 epochs respectively, separated by approximately one month to a limiting magnitude J < ∼ 24 (Vega). Image subtractions including another 20 h worth of archival ISAAC/VLT data were used to search for transients with lightcurve properties consistent with redshifted supernovae, both in the new and reference data. Results. The feasibility of finding lensed supernovae in our survey was investigated using synthetic lightcurves of supernovae and several models of the volumetric type Ia and core-collapse supernova rates as a function of redshift. We also estimate the number of supernova discoveries expected from the inferred star-formation rate in the observed galaxies. The methods consistently predict a Poisson mean value for the expected number of supernovae in the survey of between N SN = 0.8 and 1.6 for all supernova types, evenly distributed between core collapse and type Ia supernovae. One transient object was found behind A1689, 0.5 from a galaxy with photometric redshift z gal = 0.6 ± 0.15. The lightcurve and colors of the transient are consistent with being a reddened type IIP supernova at z SN = 0.59. The lensing model predicts 1.4 mag of magnification at the location of the transient, without which this object would not have been detected in the near-IR ground-based search described in this paper (unlensed magnitude J ∼ 25). We perform a feasibility study of the potential for lensed supernovae discoveries with larger and deeper surveys and conclude that the use of gravitational telescopes is a very exciting path for new discoveries. For example, a monthly rolling supernova search of a single very massive cluster with the HAWK-I camera at VLT would yield > ∼ 10 lensed supernova lightcurves per year, where type Ia supernovae would constitute about half of the expected sample. Conclusions.

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Section: Type Ia Snementioning

confidence: 89%

“…Using a different method, Strolger et al (2004) compare the SFR(t) and the SNR, r Ia V (t), derived in the GOODS fields to derive the delay-time distribution with the relation…”

Section: Type Ia Snementioning

confidence: 99%

Near-IR search for lensed supernovae behind galaxy clusters

Goobar

Paech

Stanishev³

et al. 2009

A&A

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“…Our first galaxy sample contains 2422 galaxies with secure spectroscopic redshifts (z spec ) from the ESO public compilation in the Chandra Deep Field South (CDFS; Cristiani et al 2000;Croom et al 2001;Bunker et al 2003;Dickinson et al 2004;Stanway et al 2004aStanway et al , 2004bStrolger et al 2004;Szokoly et al 2004;van der Wel et al 2004;Doherty et al 2005;Le Fèvre et al 2005;Mignoli et al 2005;Ravikumar et al 2007;Popesso et al 2009;Balestra et al 2010;Silverman et al 2010;Kurk et al 2013;Vanzella et al 2014) and from Morris et al (2015). In order to obtain multiwavelength photometry for these galaxies, we cross-matched this sample with the public Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS; Grogin et al 2011;Koekemoer et al 2011) catalog for the Great Observatory Origins Deep Survey South field (GOODS-S) obtained by Guo et al (2013).…”

Section: Samplementioning

confidence: 99%

The Impact of JWST Broadband Filter Choice on Photometric Redshift Estimation

Bisigello

Caputi

Colina

et al. 2016

ApJS

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The determination of galaxy redshifts in the James Webb Space Telescope's (JWST) blank-field surveys will mostly rely on photometric estimates, based on the data provided by JWST's Near-Infrared Camera (NIRCam) at 0.6-5.0 μm and Mid Infrared Instrument (MIRI) at l m > 5.0 m. In this work we analyze the impact of choosing different combinations of NIRCam and MIRI broadband filters (F070W to F770W), as well as having ancillary data at l m < 0.6 m, on the derived photometric redshifts (z phot ) of a total of 5921 real and simulated galaxies, with known input redshifts z=0-10. We found that observations at l m < 0.6 m are necessary to control the contamination of high-z samples by low-z interlopers. Adding MIRI (F560W and F770W) photometry to the NIRCam data mitigates the absence of ancillary observations at l m < 0.6 m and improves the redshift estimation. At z=7-10, accurate z phot can be obtained with the NIRCam broadbands alone when  S N 10, but the z phot quality significantly degrades at  S N 5. Adding MIRI photometry with 1 mag brighter depth than the NIRCam depth allows for a redshift recovery of 83%-99%, depending on spectral energy distribution type, and its effect is particularly noteworthy for galaxies with nebular emission. The vast majority of NIRCam galaxies with [F150W]=29AB mag at z=7-10 will be detected with MIRI at [F560W, F770W] < 28 mag if these sources are at least mildly evolved or have spectra with emission lines boosting the mid-infrared fluxes.

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“…It is therefore fundamental to properly take into account the Type Ia SN contribution in a theoretical model of chemical evolution. A useful formalism to compute the Type Ia SN rate in galaxies was developed by Ruiz-Lapuente & Canal (1998), by originally introducing the concept of DTD in the theoretical framework (see also Strolger et al 2004;Greggio 2005). In this formalism, the Type Ia SN rate is defined as the convolution of the galaxy star formation rate (SFR) with a suitable DTD, as follows.…”

Section: The Delay Time Distribution Of Type Ia Supernovaementioning

confidence: 99%

A simple and general method for solving detailed chemical evolution with delayed production of iron and other chemical elements

Vincenzo

Matteuccí²,

Spitoni³

2016

Mon. Not. R. Astron. Soc.

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We present a theoretical method for solving the chemical evolution of galaxies, by assuming an instantaneous recycling approximation for chemical elements restored by massive stars and the Delay Time Distribution formalism for the delayed chemical enrichment by Type Ia Supernovae. The galaxy gas mass assembly history, together with the assumed stellar yields and initial mass function, represent the starting point of this method. We derive a simple and general equation which closely relates the Laplace transforms of the galaxy gas accretion history and star formation history, which can be used to simplify the problem of retrieving these quantities in the galaxy evolution models assuming a linear Schmidt-Kennicutt law. We find that -once the galaxy star formation history has been reconstructed from our assumptions -the differential equation for the evolution of the chemical element X can be suitably solved with classical methods. We apply our model to reproduce the [O/Fe] and [Si/Fe] vs. [Fe/H] chemical abundance patterns as observed at the solar neighborhood, by assuming a decaying exponential infall rate of gas and different delay time distributions for Type Ia Supernovae; we also explore the effect of assuming a nonlinear Schmidt-Kennicutt law, with the index of the power law being k = 1.4. Although approximate, we conclude that our model with the single degenerate scenario for Type Ia Supernovae provides the best agreement with the observed set of data. Our method can be used by other complementary galaxy stellar population synthesis models to predict also the chemical evolution of galaxies.

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TheHubbleHigherzSupernova Search: Supernovae toz≈ 1.6 and Constraints on Type Ia Progenitor Models

Cited by 274 publications

References 62 publications

Near-IR search for lensed supernovae behind galaxy clusters

Near-IR search for lensed supernovae behind galaxy clusters

The Impact of JWST Broadband Filter Choice on Photometric Redshift Estimation

A simple and general method for solving detailed chemical evolution with delayed production of iron and other chemical elements

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