Searching for supernovae in the multiply-imaged galaxies behind the gravitational telescope A370

Aims. Strong lensing by massive galaxy clusters can provide magnification of the flux and even multiple images of the galaxies that lie behind them. This phenomenon facilitates observations of high-redshift supernovae (SNe) that would otherwise remain undetected. Type Ia supernovae (SNe Ia) detections are of particular interest because of their standard brightness, since they can be used to improve either cluster lensing models or cosmological parameter measurements. Methods. We present a ground-based, near-infrared search for lensed SNe behind the galaxy cluster Abell 370. Our survey was based on 15 epochs of J-band observations with the HAWK-I instrument on the Very Large Telescope (VLT). We use Hubble Space Telescope (HST) photometry to infer the global properties of the multiply-imaged galaxies. Using a recently published lensing model of Abell 370, we also present the predicted magnifications and time delays between the images. Results. In our survey, we did not discover any live SNe from the 13 lensed galaxies with 47 multiple images behind Abell 370. This is consistent with the expectation of 0.09 ± 0.02 SNe calculated based on the measured star formation rate. We compare the expectations of discovering strongly lensed SNe in our survey and that performed with HST during the Hubble Frontier Fields (HFF) programme. We also show the expectations of search campaigns that can be conducted with future facilities, such as the James Webb Space Telescope (JWST) or the Wide-Field Infrared Survey Telescope (WFIRST). We show that the NIRCam instrument aboard the JWST will be sensitive to most SN multiple images in the strongly lensed galaxies and thus will be able to measure their time delays if observations are scheduled accordingly.

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Substellar and low-mass dwarf identification with near-infrared imaging space observatories

Astronomy and Astrophysics ◽

10.1051/0004-6361/201832838 ◽

2018 ◽

Vol 620 ◽

pp. A132 ◽

Cited By ~ 4

Author(s):

B. W. Holwerda ◽

J. S. Bridge ◽

R. Ryan ◽

M. A. Kenworthy ◽

N. Pirzkal ◽

...

Keyword(s):

Near Infrared ◽

Infrared Imaging ◽

High Redshift ◽

Brown Dwarfs ◽

Wide Field ◽

Space Telescope ◽

Low Mass ◽

Space Observatories ◽

Broad Type ◽

Selection Of

Aims. We aim to evaluate the near-infrared colors of brown dwarfs as observed with four major infrared imaging space observatories: the Hubble Space Telescope (HST), the James Webb Space Telescope (JWST), the Euclid mission, and the WFIRST telescope. Methods. We used the SPLAT SPEX/ISPEX spectroscopic library to map out the colors of the M-, L-, and T-type dwarfs. We have identified which color–color combination is optimal for identifying broad type and which single color is optimal to then identify the subtype (e.g., T0-9). We evaluated each observatory separately as well as the narrow-field (HST and JWST) and wide-field (Euclid and WFIRST) combinations. Results. The Euclid filters perform equally well as HST wide filters in discriminating between broad types of brown dwarfs. WFIRST performs similarly well, despite a wider selection of filters. However, subtyping with any combination of Euclid and WFIRST observations remains uncertain due to the lack of medium, or narrow-band filters. We argue that a medium band added to the WFIRST filter selection would greatly improve its ability to preselect brown dwarfs its imaging surveys. Conclusions. The HST filters used in high-redshift searches are close to optimal to identify broad stellar type. However, the addition of F127M to the commonly used broad filter sets would allow for unambiguous subtyping. An improvement over HST is one of two broad and medium filter combinations on JWST: pairing F140M with either F150W or F162M discriminates very well between subtypes.

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Strongly Lensed Supernovae in Well-Studied Galaxy Clusters with the Vera C. Rubin Observatory

Symmetry ◽

10.3390/sym12121966 ◽

2020 ◽

Vol 12 (12) ◽

pp. 1966

Author(s):

Tanja Petrushevska

Keyword(s):

Galaxy Clusters ◽

High Redshift ◽

Cosmological Parameters ◽

Hubble Constant ◽

Multiple Images ◽

Strong Lensing ◽

Type Ia ◽

Ia Supernovae ◽

Massive Galaxy

Strong lensing by galaxy clusters can be used to significantly expand the survey reach, thus allowing observation of magnified high-redshift supernovae that otherwise would remain undetected. Strong lensing can also provide multiple images of the galaxies that lie behind the clusters. Detection of strongly lensed Type Ia supernovae (SNe Ia) is especially useful because of their standardizable brightness, as they can be used to improve either cluster lensing models or independent measurements of cosmological parameters. The cosmological parameter, the Hubble constant, is of particular interest given the discrepancy regarding its value from measurements with different approaches. Here, we explore the feasibility of the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) of detecting strongly lensed SNe in the field of five galaxy clusters (Abell 1689 and Hubble Frontier Fields clusters) that have well-studied lensing models. Considering the 88 systems composed of 268 individual multiple images in the five cluster fields, we find that the LSST will be sensitive to SNe Ia (SNe IIP) exploding in 41 (23) galaxy images. The range of redshift of these galaxies is between 1.01<z<3.05. During its 10 years of operation, LSST is expected to detect 0.2±0.1 SN Ia and 0.9±0.3 core collapse SNe. However, as LSST will observe many more massive galaxy clusters, it is likely that the expectations are higher. We stress the importance of having an additional observing program for photometric and spectroscopic follow-up of the strongly lensed SNe detected by LSST.

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Wide-Field Slitless Spectroscopy with JWST's NIRISS

Proceedings of the International Astronomical Union ◽

10.1017/s1743921315009862 ◽

2015 ◽

Vol 11 (S319) ◽

pp. 11-11

Author(s):

William V. Dixon ◽

Swara Ravindranath ◽

Chris J. Willott

Keyword(s):

Near Infrared ◽

High Redshift ◽

Galaxy Cluster ◽

Optical Emission ◽

Resolving Power ◽

Wide Field ◽

First Stars ◽

James Webb Space Telescope ◽

Infrared Imager ◽

High Redshift Universe

AbstractThe Near Infrared Imager and Slitless Spectrograph (NIRISS) aboard the James Webb Space Telescope (JWST) will offer wide-field slitless spectroscopy (WFSS) with a resolving power R = 150 at wavelengths from 0.8 to 2.25 microns. In this band, NIRISS will be sensitive to Lyman α emission lines and continuum breaks in the spectra of galaxies with redshifts 6 < z < 17, allowing it to probe the first stars and ionizing sources in the early universe. NIRISS observations of the high-redshift universe will provide a wealth of information on foreground objects, creating a unique library of optical emission-line spectra from the faintest galaxies at lower redshifts. To explore its ability to identify and characterize galaxies at all redshifts, we have modeled a NIRISS observation of a massive strong-lensing galaxy cluster and analyzed the synthetic images using standard software tools. Our simulations demonstrate that WFSS with NIRISS will provide a powerful tool for the exploration of galaxies near and far.

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See Change: VLT spectroscopy of a sample of high-redshift Type Ia supernova host galaxies

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa1319 ◽

2020 ◽

Vol 495 (4) ◽

pp. 3859-3880 ◽

Cited By ~ 1

Author(s):

S C Williams ◽

I M Hook ◽

B Hayden ◽

J Nordin ◽

G Aldering ◽

...

Keyword(s):

Hubble Space Telescope ◽

High Redshift ◽

Formation Rate ◽

Stellar Mass ◽

Light Curves ◽

Host Galaxy ◽

Host Galaxies ◽

Very Large Telescope ◽

Type Ia ◽

Ia Supernovae

ABSTRACT The Supernova Cosmology Project has conducted the ‘See Change’ programme, aimed at discovering and observing high-redshift (1.13 ≤ z ≤ 1.75) Type Ia supernovae (SNe Ia). We used multifilter Hubble Space Telescope (HST) observations of massive galaxy clusters with sufficient cadence to make the observed SN Ia light curves suitable for a cosmological probe of dark energy at z > 0.5. This See Change sample of SNe Ia with multi-colour light curves will be the largest to date at these redshifts. As part of the See Change programme, we obtained ground-based spectroscopy of each discovered transient and/or its host galaxy. Here, we present Very Large Telescope (VLT) spectra of See Change transient host galaxies, deriving their redshifts, and host parameters such as stellar mass and star formation rate. Of the 39 See Change transients/hosts that were observed with the VLT, we successfully determined the redshift for 26, including 15 SNe Ia at z > 0.97. We show that even in passive environments, it is possible to recover secure redshifts for the majority of SN hosts out to z = 1.5. We find that with typical exposure times of 3−4 h on an 8-m-class telescope we can recover ∼75 per cent of SN Ia redshifts in the range of 0.97 < z < 1.5. Furthermore, we show that the combination of HST photometry and VLT spectroscopy is able to provide estimates of host galaxy stellar mass that are sufficiently accurate for use in a mass-step correction in the cosmological analysis.

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An Efficient Approach to Obtaining Large Numbers of Distant Supernova Host Galaxy Redshifts

Publications of the Astronomical Society of Australia ◽

10.1017/pasa.2012.001 ◽

2013 ◽

Vol 30 ◽

Cited By ~ 9

Author(s):

C. Lidman ◽

V. Ruhlmann-Kleider ◽

M. Sullivan ◽

J. Myzska ◽

P. Dobbie ◽

...

Keyword(s):

High Redshift ◽

Host Galaxy ◽

Type Ia Supernovae ◽

Wide Field ◽

Host Galaxies ◽

Dark Energy Survey ◽

Large Numbers ◽

Type Ia ◽

Ia Supernovae ◽

Energy Survey

AbstractWe use the wide-field capabilities of the 2 degree field fibre positioner and the AAOmega spectrograph on the Anglo-Australian Telescope (AAT) to obtain redshifts of galaxies that hosted supernovae during the first 3 years of the Supernova Legacy Survey (SNLS). With exposure times ranging from 10 to 60 ks per galaxy, we were able to obtain redshifts for 400 host galaxies in two SNLS fields, thereby substantially increasing the total number of SNLS supernovae with host galaxy redshifts. The median redshift of the galaxies in our sample that hosted photometrically classified Type Ia supernovae (SNe Ia) is z ~ 0.77, which is 25% higher than the median redshift of spectroscopically confirmed SNe Ia in the 3-year sample of the SNLS. Our results demonstrate that one can use wide-field fibre-fed multi-object spectrographs on 4-m telescopes to efficiently obtain redshifts for large numbers of supernova host galaxies over the large areas of the sky that will be covered by future high-redshift supernova surveys, such as the Dark Energy Survey.

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All NIRspec Needs is HST/WFC3 Pre-Imaging? The Use of Milky Way Stars in WFC3 Imaging to Register NIRspec MSA Observations

Journal of Astronomical Instrumentation ◽

10.1142/s2251171716500082 ◽

2016 ◽

Vol 05 (03) ◽

pp. 1650008

Author(s):

B. W. Holwerda ◽

R. J. Bouwens ◽

M. Trenti ◽

M. A. Kenworthy

Keyword(s):

Near Infrared ◽

Hubble Space Telescope ◽

High Redshift ◽

Wide Field ◽

Galactic Latitude ◽

Space Telescope ◽

James Webb Space Telescope ◽

Specific Formula ◽

The Right ◽

Guide Star

The James Webb Space Telescope (JWST) will be an exquisite new near-infrared observatory with imaging and multi-object spectroscopy through ESA’s NIRspec instrument with its unique Micro-Shutter Array (MSA), allowing for slits to be positioned on astronomical targets by opening specific [Formula: see text]-wide micro shutter doors. To ensure proper Target Acquisition (TA), the on-sky position of the MSA needs to be verified before spectroscopic observations start. An onboard centroiding program registers the position of pre-identified guide stars in a TA image, a short pre-spectroscopy exposure without dispersion (image mode) through the MSA with all shutters open. The outstanding issue is the availability of Galactic stars in the right luminosity range for TA relative to typical high redshift targets. We explore this here using the stars and [Formula: see text] candidate galaxies identified in the source extractor catalogs of Brightest of Reionizing Galaxies survey (BoRG[z8]), a pure-parallel program with Hubble Space Telescope Wide-Field Camera 3. We find that (a) a single WFC3 field contains enough Galactic stars to satisfy the NIRspec astrometry requirement (20 milli-arcseconds), provided its and the NIRspec TA’s are [Formula: see text] AB in WFC3 [Formula: see text], (b) a single WFC3 image can therefore serve as the pre-image if need be, (c) a WFC3 mosaic and accompanying TA image satisfy the astrometry requirement at [Formula: see text] AB mag in WFC3 [Formula: see text], (d) no specific Galactic latitude requires deeper TA imaging due to a lack of Galactic stars, and (e) a depth of [Formula: see text] AB mag in WFC3 [Formula: see text] is needed if a guide star in the same MSA quadrant as a target is required. We take the example of a BoRG identified [Formula: see text] candidate galaxy and require a Galactic star within 20[Formula: see text] of it. In this case, a depth of 25.5 AB in [Formula: see text] is required (with [Formula: see text]97% confidence).

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Planck’s dusty GEMS

Astronomy and Astrophysics ◽

10.1051/0004-6361/201833679 ◽

2018 ◽

Vol 620 ◽

pp. A60 ◽

Cited By ~ 6

Author(s):

R. Cañameras ◽

N. P. H. Nesvadba ◽

M. Limousin ◽

H. Dole ◽

R. Kneissl ◽

...

Keyword(s):

Star Formation ◽

Near Infrared ◽

Infrared Imaging ◽

High Redshift ◽

Dust Emission ◽

Galaxy Cluster ◽

Star Forming ◽

The Galaxy ◽

Mass Outflow ◽

Gas Accretion

We report the discovery of a molecular wind signature from a massive intensely star-forming clump of a few 109 M⊙, in the strongly gravitationally lensed submillimeter galaxy “the Emerald” (PLCK_G165.7+49.0) at z = 2.236. The Emerald is amongst the brightest high-redshift galaxies on the submillimeter sky, and was initially discovered with the Planck satellite. The system contains two magnificient structures with projected lengths of 28.5″ and 21″ formed by multiple, near-infrared arcs, falling behind a massive galaxy cluster at z = 0.35, as well as an adjacent filament that has so far escaped discovery in other wavebands. We used HST/WFC3 and CFHT optical and near-infrared imaging together with IRAM and SMA interferometry of the CO(4–3) line and 850 μm dust emission to characterize the foreground lensing mass distribution, construct a lens model with LENSTOOL, and calculate gravitational magnification factors between 20 and 50 in most of the source. The majority of the star formation takes place within two massive star-forming clumps which are marginally gravitationally bound and embedded in a 9 × 1010 M⊙, fragmented disk with 20% gas fraction. The stellar continuum morphology is much smoother and also well resolved perpendicular to the magnification axis. One of the clumps shows a pronounced blue wing in the CO(4–3) line profile, which we interpret as a wind signature. The mass outflow rates are high enough for us to suspect that the clump might become unbound within a few tens of Myr, unless the outflowing gas can be replenished by gas accretion from the surrounding disk. The velocity offset of –200 km s−1 is above the escape velocity of the clump, but not that of the galaxy overall, suggesting that much of this material might ultimately rain back onto the galaxy and contribute to fueling subsequent star formation.

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Spectra of High-Redshift Type Ia Supernovae and a Comparison with Their Low-Redshift Counterparts

The Astronomical Journal ◽

10.1086/497635 ◽

2005 ◽

Vol 130 (6) ◽

pp. 2788-2803 ◽

Cited By ~ 44

Author(s):

I. M. Hook ◽

D. A. Howell ◽

G. Aldering ◽

R. Amanullah ◽

M. S. Burns ◽

...

Keyword(s):

High Redshift ◽

Type Ia Supernovae ◽

Type Ia ◽

Ia Supernovae

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The Hyper Suprime-Cam SSP transient survey in COSMOS: Overview

Publications of the Astronomical Society of Japan ◽

10.1093/pasj/psz050 ◽

2019 ◽

Vol 71 (4) ◽

Cited By ~ 8

Author(s):

Naoki Yasuda ◽

Masaomi Tanaka ◽

Nozomu Tominaga ◽

Ji-an Jiang ◽

Takashi J Moriya ◽

...

Keyword(s):

Light Curve ◽

Deep Layer ◽

High Redshift ◽

Galactic Nuclei ◽

Variable Stars ◽

Photometric Redshifts ◽

Data Set ◽

Type Ia ◽

Strategic Program ◽

Ia Supernovae

Abstract We present an overview of a deep transient survey of the COSMOS field with the Subaru Hyper Suprime-Cam (HSC). The survey was performed for the 1.77 deg2 ultra-deep layer and 5.78 deg2 deep layer in the Subaru Strategic Program over six- and four-month periods from 2016 to 2017, respectively. The ultra-deep layer reaches a median depth per epoch of 26.4, 26.3, 26.0, 25.6, and 24.6 mag in g, r, i, z, and y bands, respectively; the deep layer is ∼0.6 mag shallower. In total, 1824 supernova candidates were identified. Based on light-curve fitting and derived light-curve shape parameter, we classified 433 objects as Type Ia supernovae (SNe); among these candidates, 129 objects have spectroscopic or COSMOS2015 photometric redshifts and 58 objects are located at z > 1. Our unique data set doubles the number of Type Ia SNe at z > 1 and enables various time-domain analyses of Type II SNe, high-redshift superluminous SNe, variable stars, and active galactic nuclei.

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Model-independent cosmic acceleration and redshift-dependent intrinsic luminosity in type-Ia supernovae

Astronomy and Astrophysics ◽

10.1051/0004-6361/201833032 ◽

2019 ◽

Vol 625 ◽

pp. A15 ◽

Cited By ~ 8

Author(s):

I. Tutusaus ◽

B. Lamine ◽

A. Blanchard

Keyword(s):

Spline Interpolation ◽

High Redshift ◽

Cosmic Acceleration ◽

Expansion Rate ◽

Type Ia Supernovae ◽

Type Ia ◽

Model Independent ◽

Ia Supernovae ◽

The Universe ◽

Intrinsic Luminosity

Context. The cosmological concordance model (ΛCDM) is the current standard model in cosmology thanks to its ability to reproduce the observations. The first observational evidence for this model appeared roughly 20 years ago from the type-Ia supernovae (SNIa) Hubble diagram from two different groups. However, there has been some debate in the literature concerning the statistical treatment of SNIa, and their stature as proof of cosmic acceleration. Aims. In this paper we relax the standard assumption that SNIa intrinsic luminosity is independent of redshift, and examine whether it may have an impact on our cosmological knowledge and more precisely on the accelerated nature of the expansion of the universe. Methods. To maximise the scope of this study, we do not specify a given cosmological model, but we reconstruct the expansion rate of the universe through a cubic spline interpolation fitting the observations of the different cosmological probes: SNIa, baryon acoustic oscillations (BAO), and the high-redshift information from the cosmic microwave background (CMB). Results. We show that when SNIa intrinsic luminosity is not allowed to vary as a function of redshift, cosmic acceleration is definitely proven in a model-independent approach. However, allowing for redshift dependence, a nonaccelerated reconstruction of the expansion rate is able to fit, at the same level of ΛCDM, the combination of SNIa and BAO data, both treating the BAO standard ruler rd as a free parameter (not entering on the physics governing the BAO), and adding the recently published prior from CMB observations. We further extend the analysis by including the CMB data. In this case we also consider a third way to combine the different probes by explicitly computing rd from the physics of the early universe, and we show that a nonaccelerated reconstruction is able to nicely fit this combination of low- and high-redshift data. We also check that this reconstruction is compatible with the latest measurements of the growth rate of matter perturbations. We finally show that the value of the Hubble constant (H0) predicted by this reconstruction is in tension with model-independent measurements. Conclusions. We present a model-independent reconstruction of a nonaccelerated expansion rate of the universe that is able to fit all the main background cosmological probes nicely. However, the predicted value of H0 is in tension with recent direct measurements. Our analysis points out that a final reliable and consensual value for H0 is critical to definitively prove cosmic acceleration in a model-independent way.

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