Supernovae in the InfraRed Avec Hubble

XIV.0 Reunión científica 13-15 julio 2020

The aging (early spectral evolution) of SN 2020jgl (Xarel•lo) and the quest for baby supernovae with GTC

Supernovae in the InfraRed Avec Hubble

Lluís Galbany

MSCA-IF, U. Grananda

Type Ia supernovae (SNe Ia) are the most precise extragalactic distance indicators to date. Empirical relations between peak magnitude, light curve stretch and color , allow the standardisation of their optical peak magnitudes down to ~0.08mag.

XIV.0 Reunión científica 13-15 julio 2020

Type Ia supernova cosmology in the near infrared

SN Ia are more natural standard candles in the near infrared (NIR). Both theoretically and empirically, it has been found that NIR SN Ia peak magnitudes are similar down to ~0.11 mag (in H-band).

The main reason for the reduced scatter is dust extinction mitigation at NIR wavelengths.

m corr B = m obs B + ↵ x1 c

L um inos it y !

Time!

Δm₁₅

15 days

Time from maximum brightness

A b so lut e m ag nit ud e

(⌦

_M

, ⌦

_⇤

, w)

(0.3, 0.0, 0.0) (1.0, 0.0, 0.0)

(0.32, 0.68, 0.98)

Brout et al. (2019) Kim et al. (1997)

Avelino et al. (2019)

Cardelli et al. (1989) Kasen et al. (2006)

However, there is a lack of SN

Ia observations in the NIR…

XIV.0 Reunión científica 13-15 julio 2020

HST Cycles 27 and 28 approved program to obtain NIR observations of 24 Hubble-flow (0.02 < z < 0.07) SN Ia with WFC3/IR [2 objects per month Feb 20-21]

independent of SN Ia!

66 68 70 72 74 76

H

₀

(km sec

^-1

Mpc

^-1

)

Planck 2018 (ΛCDM) Planck 2016 (ΛCDM)

Riess+ 2016

C17, F18, FK18 reanalyses

Burns+ 2018 NIR+optical Dhawan+ 2018 SN Ia NIR only

SIRAH forecast

Riess+ 2019 +LMC EBs Freedman+ 2019 CCHP TRGB

Reid+ 2019 N4258 TRGB

Wong+ 2019 H0LICOW lenses Pesce+ 2020 masers

∆ w₀ = -0.1

∆ w_a = -1

∆ N_eff = +0.4

∆ Ω_K = -0.01

∆ σ = 10^-33 cm²/g

new physics

«

»

(beyond

Λ CDM)

Discovery: building on SN search surveys (ZTF, ATLAS, PS, ASASSN) and public brokers (ALeRCE, Lasair, Anteres)

10

^-18

10

^-17

10

^-16

10

^-15

observed flux (erg/cm

2

/s/A)

10

^-18

10

^-17

10

^-16

10

^-15

observed flux (erg/cm

2

/s/A)

8000 10000 12000 14000 16000 observed wavelength (A)

10 100

SNR per pixel

8000 10000 12000 14000 16000 observed wavelength (A)

10 100

SNR per pixel

200

50 20

5

G102 grism 2x450s G141 grism 2x400s brightest:

z = 0.02 SN Ia at max J = 16.0, H = 16.2

faintest:

z = 0.07 SN Ia at +10d J = 19.5, H = 19.6

brightest

faintest

atmospheric absorption

Figure 3: Simulated WFC3/IR grism observations based on the HST WFC3 ETC spanning the range of our brightest (top) and faintest (bottom) Hubble-flow objects. The vertical gray bands show the regions heavily a↵ected by atmospheric absorption in ground-based data. The input spectrum (dark gray) is based on SN 2011fe from Hsiao+ (2013). The lower panel shows the signal-to-noise ratio (SNR) expected in each extracted pixel for the brightest and faintest Hubble-flow targets; these should bracket all of our Hubble-flow data.

7

10

^-18

10

^-17

10

^-16

10

^-15

observed flux (erg/cm

2

/s/A)

10

^-18

10

^-17

10

^-16

10

^-15

observed flux (erg/cm

2

/s/A)

8000 10000 12000 14000 16000 observed wavelength (A)

10 100

SNR per pixel

8000 10000 12000 14000 16000 observed wavelength (A)

10 100

SNR per pixel

200

50 20

5

G102 grism 2x450s G141 grism 2x400s brightest:

z = 0.02 SN Ia at max J = 16.0, H = 16.2

faintest:

z = 0.07 SN Ia at +10d J = 19.5, H = 19.6

brightest

faintest

atmospheric absorption

Figure 3: Simulated WFC3/IR grism observations based on the HST WFC3 ETC spanning the range of our brightest (top) and faintest (bottom) Hubble-flow objects. The vertical gray bands show the regions heavily a↵ected by atmospheric absorption in ground-based data. The input spectrum (dark gray) is based on SN 2011fe from Hsiao+ (2013). The lower panel shows the signal-to-noise ratio (SNR) expected in each extracted pixel for the brightest and faintest Hubble-flow targets; these should bracket all of our Hubble-flow data.

7

Supernova in the InfraRed Avec Hubble

Around 2 week turnaround for HST: we need to trigger on very young SN Ia (few days post explosion) want near-max data.

Classification: relying on ground-base ToO programs with large aperture telescopes (e.g. GTC!)

2 epochs of grism spectroscopy: G102, G141

Photometry in 5 NIR bands: F098M, F105W, F125W, F140W, F160W

3 key science goals: ✶ rest-frame NIR SEDs for WFIRST


✶ 2.7% NIR SN Ia H 0 measurement


✶ HST Hubble diagram to z = 0.6 (w/RAISINs; high-z)

Jha et al. (2019)

PI: Saurabh Jha (Rutgers)

XIV.0 Reunión científica 13-15 julio 2020

1.Surveys discover SN candidates

HST WFC3/IR G102+G141 UT 2020-02-17 data reduction by Russell Ryan (STScI)

SN 2020bpi

F160W G102 grism

wavelength (µm) 100

flux density ( µ Jy)

20 50 200

0.8 0.9 1.0 1.2 1.4 1.6

first ever rest-frame NIR spectrum of a maximum light SN Ia from space!

2. Brokers classify and organise these discoveries

3. SIRAH searches for good young SNIa candidates from brokers

Science Template Difference

5. If a young SNIa, HST is triggered!

Mi Dai (Rutgers)

4. ToO programs request spectra to classify the best candidates

4000 5000 6000 7000 8000 9000 Rest-frame wavelength [˚A]

°16

°14

°12

°10

°8

Log(Flux)+ct

©

© GTC -16.1 d

SALT -15.2 d GTC -15.1 d GTC -14.1 d LCOGT -12.6 d GSP -12.5 d GSP -10.6 d LCOGT -9.6 d GSP -8.7 d LCOGT -3.8 d LT -3.2 d LT -0.2 d GSP 0.3 d UCB 1.1 d GSP 4.3 d UCB 5.1 d GSP 11.2 d SALT 13.6 d GSP 19.2 d GSP 37.0 d

3.6 3.8 4.0 4.2 4.4

log(Rest-frame [A])

−18

−17

−16

−15

−14

log(F)

GSP -10.6 d SpeX -10.8 d GSP 0.3 d SpeX 0.1 d UCB 1.1 d HST 2.5 d

XIV.0 Reunión científica 13-15 julio 2020

Proposal GTC52-20A (PI: Lluís Galbany):

Follow-up of infant SNe within 48h from explosion

SN name Type Time from discovery

ZTF20aaxvzja - SN2020itj II 15h 05.84m ZTF20aaynrrh - SN2020jfo II 16h 51.43m ATLAS20lti - SN2020jgl Ia 14h 34.39m ATLAS20lts - SN2020jhf Ia-91bg 1d 11h 48.75m ZTF20abaovyz - SN2020kjt II 18h 58.49m ZTF20abapyxl - SN2020kku Ia 18h 28.06m ZTF20abbhyxu - SN2020kyx Ia 22h 02.15m ZTF20abazeye - AT2020krl CV 3d 17h 44.88m ZTF20abbplei - SN2020lao IcBL 18h 45.72m ZTF20abisitz - SN2020nny II 17h 12.89m

10 classifications of SN candidates

Triggered by SIRAH

Papers in preparation

°20 °10 0 10 20 30 40 50

Rest-frame epoch from B-band maxi um [day]

10

12

14

16

18

20

Apparentmagnitude[mag]

U+1 B V-1 g-2 r-3 i-4

Las Cumbres telescope network UBVgri photometry

SpeX + HST NIR spectroscopy

Optical spectroscopic sequence from: GTC + SALT + Las Cumbres +

Liverpool + KAIT

9

^h

29

^m

02

^s

00

^s

28

^m

58

^s

56

^s

° 14

^±

47

⁰

30

⁰⁰

48

⁰

00

⁰⁰

30

⁰⁰

49

⁰

00

⁰⁰

Right Ascension (J2000)

Declination (J2000) SN

SN 2020jgl

12 spectra pre-max

(more to come…)

GTC/OSIRIS

XIV.0 Reunión científica 13-15 julio 2020

Impact and prospects for the future

- Continuing GTC-OSIRIS program for the classification of very young SNe, and allow further follow up that lead to individual studies of the most interesting objects

- New GTC-EMIR program to complement NIR spectroscopy of SIRAH targets and enable SNIa subtyping

- New NOT/TNG program to complement NIR photometry of SIRAH targets to better

populate the H-band light curve, and also provide J-band with prospect of constructing a J and H-band independent Hubble diagrams.

- Long-term project: The Carnegie Supernova Project (CSP III) will be focused on the study of infant SNe, starting in mid 2021, right after SIRAH observations are finished.

- Enhance the participation of Spanish researchers/institutions in SN physics/cosmology

international collaborations (SIRAH, CSP , DES, LSST-DESC…)