Gerlumph Data Release 2:2.5 Billion Simulated Microlensing Light Curves

Vernardos, G.; Fluke, C. J.; Bate, N. F.; Croton, Darren J.; Vohl, Dany

doi:10.1088/0067-0049/217/2/23

Cited by 29 publications

(27 citation statements)

References 66 publications

(109 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…To calculate microlensed light curves, we use the emitted specific intensity I λ,e (t, p) at the source plane calculated via ARTIS for a given SN model, where I λ,e (t, p) is a function of wavelength λ, time since explosion t, and impact parameter p, which is the projected distance from the ejecta center. We combine I λ,e (t, p) with magnification maps from GERLUMPH (Vernardos et al 2015;Chan, in prep. ), which uses the inverse ray-shooting technique (e.g., Kayser et al 1986;Wambsganss et al 1992;Vernardos & Fluke 2013) yielding the magnification factor µ(x, y) as a function of cartesian coordinates x and y on the source plane 2 .…”

Section: Microlensing On Sne Iamentioning

confidence: 99%

Holismokes

Huber

Suyu

Noebauer

et al. 2021

A&A

View full text Add to dashboard Cite

To use strongly lensed Type Ia supernovae (LSNe Ia) for cosmology, a time-delay measurement between the multiple supernova (SN) images is necessary. The sharp rise and decline of SN Ia light curves make them promising for measuring time delays, but microlensing can distort these light curves and therefore add large uncertainties to the measurements. An alternative approach is to use color curves where uncertainties due to microlensing are significantly reduced for a certain period of time known as the achromatic phase. In this work, we investigate in detail the achromatic phase, testing four different SN Ia models with various microlensing configurations. We find on average an achromatic phase of around three rest-frame weeks or longer for most color curves, but the spread in the duration of the achromatic phase (due to different microlensing maps and filter combinations) is quite large and an achromatic phase of just a few days is also possible. Furthermore, the achromatic phase is longer for smoother microlensing maps and lower macro-magnifications. From our investigations, we do not find a strong dependency on the SN model or on asymmetries in the SN ejecta. We find that six rest-frame LSST color curves exhibit features such as extreme points or turning points within the achromatic phase, which make them promising for time-delay measurements; however, only three of the color curves are independent. These curves contain combinations of rest-frame bands u, g, r, and i, and to observe them for typical LSN Ia redshifts, it would be ideal to cover (observer-frame) filters r, i, z, y, J, and H. If follow-up resources are restricted, we recommend r, i, and z as the bare minimum for using color curves and/or light curves since LSNe Ia are bright in these filters and observational uncertainties are lower than in the infrared regime. With additional resources, infrared observations in y, J, and H would be useful for obtaining color curves of SNe, especially at redshifts above ∼0.8 when they become critical.

show abstract

Section: Microlensing On Sne Iamentioning

confidence: 99%

Holismokes

Huber

Suyu

Noebauer

et al. 2021

A&A

View full text Add to dashboard Cite

show abstract

“…where the emitted specific intensity, I λ,e (t, x, y), is multiplied with the microlensing magnification map 4 µ(x, y) from GERLUMPH (Vernardos et al 2015;Chan et al 2020) and integrated over the whole size of the projected SN Ia. The specific intensity I λ,e (t, x, y) depends on the time since explosion t, the wavelength λ, and the radial coordinate on the source plane p = x 2 + y 2 , given our spherical averaging of the photon packets from the models 5 .…”

Section: Microlensing Formalism and Mapsmentioning

confidence: 99%

Holismokes

Suyu

Huber

Cañameras

et al. 2020

A&A

View full text Add to dashboard Cite

We present the HOLISMOKES programme on strong gravitational lensing of supernovae (SNe) as a probe of SN physics and cosmology. We investigate the effects of microlensing on early-phase SN Ia spectra using four different SN explosion models. We find that distortions of SN Ia spectra due to microlensing are typically negligible within ten rest-frame days after a SN explosion (< 1% distortion within the 1σ spread and ≲10% distortion within the 2σ spread). This shows the great prospects of using lensed SNe Ia to obtain intrinsic early-phase SN spectra for deciphering SN Ia progenitors. As a demonstration of the usefulness of lensed SNe Ia for cosmology, we simulate a sample of mock lensed SN Ia systems that are expected to have accurate and precise time-delay measurements in the era of the Rubin Observatory Legacy Survey of Space and Time (LSST). Adopting realistic yet conservative uncertainties on their time-delay distances and lens angular diameter distances, of 6.6% and 5%, respectively, we find that a sample of 20 lensed SNe Ia would allow us to constrain the Hubble constant (H0) with 1.3% uncertainty in the flat ΛCDM cosmology. We find a similar constraint on H0 in an open ΛCDM cosmology, while the constraint degrades to 3% in a flat wCDM cosmology. We anticipate lensed SNe to be an independent and powerful probe of SN physics and cosmology in the upcoming LSST era.

show abstract

“…Due to conservation of energy, microlensing by stars does not change the average magnification over an ensemble, but it can introduce significant scatter (Dobler & Keeton 2006;Foxley-Marrable et al 2018;Goldstein et al 2018). We use the microlensing magnification distributions from Vernardos et al (2014Vernardos et al ( , 2015 to build the probability density function for microlensing magnification. For simplicity sake, we assume all trailing images go through the region star field where 80 per cent of the mass is in stars and 20 per cent in a smooth (dark matter) component.…”

Section: Type Iip Shock Breakoutmentioning

confidence: 99%

Observing the earliest moments of supernovae using strong gravitational lenses

Foxley-Marrable

Collett

Frohmaier

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We determine the viability of exploiting lensing time delays to observe strongly gravitationally lensed supernovae (gLSNe) from first light. Assuming a plausible discovery strategy, the Legacy Survey of Space and Time (LSST) and the Zwicky Transient Facility (ZTF) will discover ∼110 and ∼1 systems per year before the supernova (SN) explosion in the final image, respectively. Systems will be identified $11.7^{+29.8}_{-9.3}$ d before the final explosion. We then explore the possibility of performing early-time observations for Type IIP and Type Ia SNe in LSST-discovered systems. Using a simulated Type IIP explosion, we predict that the shock breakout in one trailing image per year will peak at ≲24.1 mag (≲23.3) in the B-band (F218W), however evolving over a time-scale of ∼30 min. Using an analytic model of Type Ia companion interaction, we find that in the B-band we should observe at least one shock cooling emission event per year that peaks at ≲26.3 mag (≲29.6) assuming all Type Ia gLSNe have a 1 M⊙ red giant (main sequence) companion. We perform Bayesian analysis to investigate how well deep observations with 1 h exposures on the European Extremely Large Telescope would discriminate between Type Ia progenitor populations. We find that if all Type Ia SNe evolved from the double-degenerate channel, then observations of the lack of early blue flux in 10 (50) trailing images would rule out more than 27 per cent (19 per cent) of the population having 1 M⊙ main sequence companions at 95 per cent confidence.

show abstract

Gerlumph Data Release 2:2.5 Billion Simulated Microlensing Light Curves

Cited by 29 publications

References 66 publications

Holismokes

Holismokes

Holismokes

Observing the earliest moments of supernovae using strong gravitational lenses

Contact Info

Product

Resources

About