A smooth ride through SN II cosmology?

adcc

Stefan Taubenberger (MPA)
on behalf of the adH0cc team

H0 - the early days
Edwin Hubble, 1929:
the more distant agalaxy is, the morestrongly redshifted
is its light
500 km/s
Theoretical workby GeorgesLemaître (1927,1931): Universeis expanding
2

1 Mpc

H0 - 90 years of controversy
https://www.cfa.harvard.edu/~dfabricant/huchra/hubble/

HST key project3

H0 - 90 years of controversy

Local distance ladder

Early Universe (CMB)[Freedman 2017]
4

BUTLateUniverse

lots of efforts
to solve it
5

H0 [km/s/Mpc]

Image: A. Holas (adapted from di Valentino 2021)

H0 tension

EarlyUniverseToo many cooks spoil the soup?
Image: https://twitter.com/cartoonlka

Distance ladder – SH0ESus?
Masers – MCP

Lensed quasars – H0LiCOWCMB – Planck6

Too many cooks spoil the soup?
Precision?

< 2 - 3%
Cosmological-model
independent?

z < 0.15
Absolute distances?

7

✓
✓✗

Distance ladder – SH0ES

Absolutedistancedistance
ladderphysical model

empirical modelToo many cooks spoil the soup?
Precision?

< 2 - 3%Cosmological-modelindependent?

z < 0.15
Absolute distances?

8✗
Masers – MCP✓✓

Too many cooks spoil the soup?
Precision?

< 2 - 3%
Cosmological-modelindependent?

✓✗z < 0.15
Absolute distances?

9✓

Lensing – H0LICOW

Too many cooks spoil the soup?
Precision?

< 2 - 3%
Cosmological-modelindependent?

z < 0.15
Absolute distances?

10

✓
✓
✓

ad Hocsolution

ad< 2 - 3%z < 0.15

11a ccurated eterminationof H0orefrom c razyollapsec osmologists
supernovaeccS. Smartt
R. KotakC. Lemon
A. Gal-Yam
R. Bruch12ad

cc - TeamJ. Spyromilio
S. Blondin
B. Leibundgut
S. Suyu
C. VoglA. Floers
S. Taubenberger
M. G. Cudmani
A. HolasW. Hillebrandt
G. Csoernyei
S. Kressierer

Why type II supernovae?
Luminosity ~ Period

Type II supernovae

Type II supernovae:
simplephysics

SN II:

luminosity
Luminosity~ light curve width
directly
frommodelsone-stepmeasurement

Riess et al. 201613

physics
basedType II supernovae: emission
Expanding-Photosphere
Methodcorehydrogen envelope
photosphereshock
depositedenergy14EPM in a nutshell

Image: Héloïse Stevance

Image: NASA Kepler/K215

SNEPM in a nutshell

16

EPM in a nutshell

SN17

EPM: reality check
Supernova is not ablackbody!

Line features

Flux = 15 %blackbody flux

18

Distances from spectral fits
Spectral-fitting Expanding Atmosphere Method
Baron et al. (95, 96, 2004, 2007), Lentz et al. 2001, Mitchell et al. 2002

Tailored Expanding Photosphere Method
Dessart et al. (2006, 2008)

:ot
edilp
apylno→X,ρ,…
wodllfetatealoctbilbnpiuImI
HoeeChNtSni
3
IIeoN
S0o

[Baron et al. 2004]
19

Luminosity

TARDIS
Kerzendorf & Sim 2014
Monte CarloBlackbody
Inner
Boundary

Improved for Type II SNe:bound-free, free-free,collisional processes

NLTE and thermal
structure…

Vogl et al. (2019)20

Does TARDIS work?

21

Parameter inference

XFe,…
Traditional method:

vph

Tph

LλOptimization by hand and eye (e.g., Dessart & Hillier 2006, 2008)
Advantages:
uses spectroscopist’s
knowledge
22Drawbacks:
infeasible for large datasetsnot reproducible
no uncertainties

Spectral emulation

107 times faster~ 1 day per simulation

Emulate instead of simulate
e.g. Heitmann
etal.
2009,
Czekalaetal.
2015,
Lietzau
2017
i.e. interpolate on a grid of pre-computed spectra

Reasoning:

Spectra vary smoothly with the parameters
Interpolation uncertainties < 1% in most spectral bins (Vogl et al. 2020)23

H0 from type II supernovae
SN 2013fs

SN 2006it💥

iPTF13bjx

💥

💥

z
0.01

0.02

SN 2003bn💥

24

SN 2010id💥

0.030.04
SN 2012ck
💥

H0 – Distances

iPTF13bjx
💥

25

H0 – ResultsiPTF13bjx
💥

imiler!
yranP

26

Data 2.0mk004

Distance precision ≈10-15 %/s

z0.01

0.04

0.08

13 %

3.3 %

1.3 %

Distance precision < 10 %< 30 d after explosion

H0 uncertainty

H0 precision ≈ 2 % ≈ 10 % / 25 0.5
27

individual H0 precision# of objects 💥

Data 2.0xm
k004

Distance precision < 10 %/s< 30 d after explosion

z0.01
13 %

0.04

0.08

3.3 %

1.3 %

Well calibrated
spectraH0 uncertainty

data do n

as fewinstruments aspossible

ot exist!

H0 precision ≈ 2 % ≈ 10 % / 25 0.5
28

individual H0 precision# of objects 💥

Data 2.0 – adH0cc
Need ~15-20 SNe in this z-rangez

SN II with absolute mag -17:
0.01

0.04

0.08

16 mag

19 mag

21 magFORS2
BVRI
photometry

per SN:29

150 hoursover 1.5 yea< 30 d after explosion

rs

Image: ESO/Y. Beletsky

adH0cc - Status

START

October 2019

30END

April 2020

October 2020

October 2021

Image: ESO/Y. Beletsky

adH0cc - VLT Large Programme

31

Image: ESO/Y. Beletsky

Image: ESO/Y. Beletskyradiative transfer

peculiar extinction
Credit: Hope Ishii

circumstellar material

RV != 3.1

Radius != velocity x time

33

Credit: NAOJsitsilsThi!
etelpmocniylniatrce