localiahosts_neill

8/6/2019 LocalIaHosts_Neill

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Local SN Ia Host Properties

and their EffectsJames D. Don Neill


2/21

Outline

Define terms: local & effects

Host properties and challenges

Light curve effects

Hubble residual effects

Final thoughts


3/21

What is Local?

For integrated demographics: z < 0.1For resolved demographics: z z < 0.1

For spectral effects: high S/N spectra


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SN Ia Diversity

How do hosts connect?Hubble Diagram Residuals

Light Curve Properties:

Shape: stretch, m15, rise-time, 2ndary peak

Color: E(B-V)MAX, AV -> dust

Spectroscopic Properties:

lines: EW, velocities, polarization

continuum: mangle-factor, slope?


5/21

Host PropertiesType, SFR, M*, sSFR, Age, -> SFH

Photometry: Colors, SED, integrated, site

Fit to SFH models

Tremonti, Mannucci: M*, SFR-> [O/H] (?)

Spectroscopy:line diagnostics: SFR, [O/H], Dn(4000), HA

spectral fits: SFR, M*, Age


6/21

Local Challenges

Heterogeneous SN photometry

Local Velocity FieldSample biases

Complex SFH

Complex Host photometry

Sample size: small volume


7/21

Local SNe Ia

CfA3, Conley 10

UV - optical

integrated photometry

PEGASE.2 SFH models

Mass bias

SFR bias

Age, sSFR OK


8/21

NGC2841SN199BY

GALEXFUV,NUV

GLGA: GALEXLARGE GALAXY ATLAS

~20,000 GALAXIES, D25 > 0.8 ARCMINGALEX, SDSS, 2MASS, OTHERSCOMPARISON SAMPLE FOR SN HOSTS


9/21

NGC2841SN199BY

SDSSg,r,i

GLGA: GALEXLARGE GALAXY ATLAS


10/21

0 2 4 6 8 10Re [arc minutes]

18

17

1615

14

13

GrowthCurve

[ABmag]

APRFUV

NUV


32

30

28

26

24

22

[

ABmag/a

rcsec

2]

APR

FUV

NUV


0.4

0.5

0.6

0.7

TotalFUV!N

UV


0.4

0.6

0.8

1.0

1.2

1.4

1.6

AnnularFUV!NUV

ID: NGC2841

FUV EXPTIME [s]: 12811.7NUV EXPTIME [s]: 16590.6

R.A. [J2K]: 140.510834

DEC [J2K]: 50.976391

SEMIMAJOR [arcmin]: 9.77

RATIO (a/b): 2.11

P.A.: 147.00

TOT: m(FUVo)=13.59 m(FUVdr)=13.47 (0.03)TOT: m(NUVo)=12.99 m(NUVdr)=12.86 (0.04)

TOT: FUV!NUV=0.61 (0.05)

APR: m(FUVo)=13.68 m(FUVdr)=13.55 (0.01)

APR: m(NUVo)=13.13 m(NUVdr)=13.01 (0.02)

APR: FUV!NUV=0.54 (0.02)

BG FUV: 29.06 (0.04) BG NUV: 27.49 (0.02)

GAL E(B!V): 0.015

GAL AFUV: 0.126

GAL ANUV: 0.125

Fri May 1 10:22:45 2009

ELLIPTICAL APERTURE SURFACE PHOTOMETRY


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12/21

Light Curve Effects

Short delay - high s

Long delay - low s

2 components?

continuous?

93H complex (massive)host


13/21

Light Curve Effects

Mass - Metallicity

Metallicity - 56Ni?

Trend explained?

93H host accreteddwarf?


14/21

Mass - Metallicity


15/21

Howell et al. 09 ~ 0.7


16/21

Hubble Residuals

Low extinction (top)

Same sense as Masstrend (next slide)


17/21

Hubble Residuals

Same trend as in Sullivan 10, Lampeitl 10

Kelly et al. 10


18/21

UV Makes it Better

Kelly et al. 10

UV host photometry improves host masses?


19/21

Local Improvements

Large sample with uniform SN Ia photometry

PTF, PanSTARRS, CSP, etc.

Better bolometric maxima

Better56

Ni mass estimatesStretch-lum for low stretch SNe


20/21

Local Improvements

Uniform host photometry

More with SDSS-like photometry

Better host metallicities

Mannucci (10) improvement to Tremonti

Look again at HR vs [O/H]Scanning spectroscopy of local hosts

expensive in telescope time


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Host Offerings

Age, metallicity must be primary causes forLcur, HR trends

Host mass cannot be known by progenitor

SN Ia timescale prevents direct sitecorrelation -> radial correlations might work

Look for SN spectroscopy trends

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