strategies to identify strongly lensed type Ia supernovae in the rubin LSST

Prajakta Mane

Final year, Integrated BS-MS,

Indian Institute of Science Education and Research (IISER) Mohali, India

LSST TDWG Meeting

Anupreeta More, Surhud More

Inter-University Centre for Astronomy and Astrophysics (IUCAA), India

March 26, 2024

Time delay cosmography:

\frac{D_d D_s}{D_{ds}} = \frac{1}{H_0} f(z_s, z_l, \Omega_m, \Omega_\Lambda )
\Delta t = \frac{D_d D_s}{cD_{ds}}(1+z_l)\Delta\tau \text{+ constant}

accurate time delays, surface mass distribution and redshift of lens

Hubble constant with strong lensing time delays

well-constrained Hubble Constant!

Hubble constant constraints from 6 lensed quasars, Wong et al., 2019

Time delay cosmography:

\frac{D_d D_s}{D_{ds}} = \frac{1}{H_0} f(z_s, z_l, \Omega_m, \Omega_\Lambda )

accurate time delays, surface mass distribution and redshift of lens

Hubble constant with strong lensing time delays

well-constrained Hubble Constant

What makes SNeIa a better source for TDC?

  • well-studied light curves -> more accurate time delay measurements

  • transient source -> improved constraints on the lens galaxy model

  • standard candle nature -> help overcome degeneracies

How to find lensed SNeIa?

DIA: run LSST Stack's difference imaging pipeline to identify multiply imaged SNe

CMA: study outliers in the colour-magnitude space for transients to identify lensed SNeIa

  • Raw exposures from Subaru Hyper-Suprime Cam (HSC) -> Public Data Release 1
  • UltraDeep Survey's COSMOS region, Tract number 9813 (~1.7 deg wide)
  • 149 visits in grizy from 10 nights in 2014 and 2015: 16,688 CCD images
  • LSST Science Pipeline w_2022_12
  • Strong lensing positions, magnifications, and time delays simulated using a code adapted from More & More, 2022
  • SNe light curves: SALT2 (Guy et al., 2007, 2010) template built in SNCosmo (Barbary et al., 2017) manually incorporating strong lensing observables

SNe light curve simulations

Sky data for DIA

Difference imaging analysis

Preliminary results

Difference imaging analysis

Preliminary results

  • Total recovery fraction ~70%​​
  • Slightly higher for quads
  • Decreases significantly for the y-band
Injected Detected % recovery
Total 74k 51.5k 70
Doubles 70k 48.3k 70
Quads 4.1k 3.2k 78
g 310 260 83
r 5.4k 4.7k 86
i 14k 11k 80
z 21k 16k 76
y 34k 20k 58

Difference imaging analysis

Preliminary results

Recovery fraction variation with injected unresolved magnitude

Recovery fraction variation with maximum injected angular separation

  • Recovery fraction decreases for fainter systems.
  • Expected variation across different bands both with magnitude and angular separation.

Color-magnitude analysis

Quimby et al. 2014

         : Unlensed SNIa

         : Unlensed core collapse

         : Lensed SNIa
         : Lensed core collapse

 

The redder supernovae for given i-band magnitude are more likely to be lensed SNeIa

High redshift: 1.64 < z < 2.4

CM diagram for simulated SNeIa

The black bold curve separates the lensed SNeIa from unlensed both on the rising and the falling edge of light curve for z < 2.4!

Low redshift: z < 1.64

Comparison with observed SNeIa

The criteria hold well for the observed unlensed and lensed SNeIa!

Contamination from SNcc (Simulated)

Unlensed

Lensed

Not too much! Lensed Ib and Ic are majority of contaminants

Summary of current results

  • Employed differece imaging pipeline recovers ~70% of the injected data of lensed SNeIa.
  • Colour-magnitude criteria hold well for simulated and observed (un-)lensed SNeIa till redshift 2.4, both on rising and falling edge. Contamination from (un-)lensed SNeCC is low.

Thank you!

Ongoing work

  • Separate DIA sources detected as resolved and unresolved by the pipeline and study their recovery properties.
  • Study extended DIA sources to check if extendedness can be used as a marker for a lensed system.
  • Study contamination by superluminous SNe in the CM space of lensed SNeIa.

Time delay cosmography:

\frac{D_d D_s}{D_{ds}} = \frac{1}{H_0} f(z_s, z_l, \Omega_m, \Omega_\Lambda )

accurate time delays, surface mass distribution and redshift of lens

Hubble constant with strong lensing time delays

well-constrained Hubble Constant

What makes SNeIa a better source for TDC?

  • well-studied light curves -> more accurate time delay measurements

  • transient source -> improved constraints on the lens galaxy model

  • standard candle nature -> help overcome degeneracies

Current lensed supernova sample

SNIa

H_0 = 66.6^{+4.1}_{-3.3}

SNIa

better constraints expected

Time delay cosmography:

\frac{D_d D_s}{D_{ds}} = \frac{1}{H_0} f(z_s, z_l, \Omega_m, \Omega_\Lambda )

accurate time delays, surface mass distribution and redshift of lens

Hubble constant with strong lensing time delays

well-constrained Hubble Constant

What makes SNeIa a better source for TDC?

  • well-studied light curves -> more accurate time delay measurements

  • transient source -> improved constraints on the lens galaxy model

  • standard candle nature -> help overcome degeneracies

How to find lensed SNeIa?

DIA: run LSST Stack's difference imaging pipeline to identify multiply imaged SNe

CMA: study outliers in the colour-magnitude space for transients to identify lensed SNeIa

H_0 = 66.6^{+4.1}_{-3.3}

better constraints expected

Current lensed supernova sample

SNIa

SNIa

Made with Slides.com