Seeing the (Infrared) Light Marco Viero KIPAC/Stanford w/ - - PowerPoint PPT Presentation

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Seeing the (Infrared) Light Marco Viero KIPAC/Stanford w/ - - PowerPoint PPT Presentation

Mar 25, 2023 387 likes •833 views

Seeing the (Infrared) Light Marco Viero KIPAC/Stanford w/ Lorenzo Moncelsi (Caltech), Ryan Quadri (Texas A&M), and the HerMES Collaboration Motivation Infrared/Submillimeter emission M reprocessed starlight by dust IR/Submm

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Seeing the (Infrared) Light

Marco Viero — KIPAC/Stanford

w/ Lorenzo Moncelsi (Caltech), Ryan Quadri (Texas A&M), and the HerMES Collaboration

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

  • How do we reconcile COB and CIB?
  • Want to know:

➡which galaxies make up CIB? ➡how much of the CIB is accounted for? ➡what limits does this place on models?

Motivation

2

M

da Cunha+2010 Dole+2006

COB CIB

1000 10 0.1 Wavelength (μm) nW m2 sr-1 0.1 100 10 1

  • Infrared/Submillimeter emission

reprocessed starlight by dust

  • IR/Submm traces star formation
  • Half the emission is tied up in dust
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SLIDE 3

marco.viero@stanford.edu Lisbon Seminar — May 3 2016

Herschel/SPIRE

  • < 1% of sources resolved at

5σ due to source confusion

  • Strength is surveys, with

~1000 deg2 observed

3

1arcmin

250 μm: 18” 350 μm: 25” 500 μm: 36”

PSF size (FWHM)

250μm contours

24.0 mJy 27.5 mJy 30.5 mJy

Confusion Limit (5σ) 3.5 M Primary Band

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

Optical v. Infrared Background

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250um z-band

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

  • Realize that

fluctuations are real signal

  • Take advantage

by modeling based on fitting to the intensities

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GOODS-S Half 1 GOODS-S Half 2

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

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18” SPIRE 250μm Beam

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Optical v. Infrared Background

  • Half the emission is tied up in dust
  • ad

SPIRE Contour

  • Difficult to attribute an individual

submillimeter “source” to any single galaxy

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SPIRE 250μm 18” Beam

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SLIDE 8

Optical v. Infrared Background

  • Half the emission is tied up in dust
  • ad

SPIRE Contour SPIRE 250μm 18” Beam

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  • Key is to identify galaxies with

similar physical properties, and then rely on statistics to fit fluctuations

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SLIDE 9

marco.viero@stanford.edu Lisbon Seminar — May 3 2016

SIMSTACK: Synthetic Intensity Fitting Algorithm

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SIMSTACK code publicly available (see arXiv:1304.0446): IDL (old) — https://web.stanford.edu/~viero/downloads.html Python (under development!) — https://github.com/marcoviero/simstack

make hits map from catalog of similar objects convolve with instrument p.s.f. regress to find mean flux density

Formalism developed w/ Lorenzo Moncelsi (Caltech); also see Kurczynski & Gawiser (2010), Roseboom et al. (2010)

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SLIDE 10

marco.viero@stanford.edu Lisbon Seminar — May 3 2016

Simplest Intensity Fitting

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RA DEC 149.853 2.608 149.854 2.258 149.752 2.584 149.832 2.724 149.275 2.196 149.262 2.966 149.915 2.206 149.546 2.564 149.824 2.047 149.453 2.278 149.863 2.788 … … … …

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SLIDE 11

marco.viero@stanford.edu Lisbon Seminar — May 3 2016

Simplest Intensity Fitting

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

SIMSTACK: Synthetic Intensity Fitting Algorithm

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× C1 × C2 × CN

+ …+ +

≈

sky map

…

sub-catalog 1 sub-catalog 2 sub-catalog N ➜ ➜ ➜ Formalism developed w/ Lorenzo Moncelsi (Caltech)

SIMSTACK code publicly available (see arXiv:1304.0446): IDL (old) — https://web.stanford.edu/~viero/downloads.html Python (under development!) — https://github.com/marcoviero/simstack

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SLIDE 13

marco.viero@stanford.edu Lisbon Seminar — May 3 2016

Aside: Correlated vs. Uncorrelated Emission

  • In a typical

thumbnail stack, uncorrelated emission does not bias result,

  • nly adds noise

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10,000 iterations

no bias

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SLIDE 14

marco.viero@stanford.edu Lisbon Seminar — May 3 2016

Aside: Correlated vs. Uncorrelated Emission

  • However

correlated emission does bias a typical thumbnail stack, increasingly with increasing beam

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Source Density (arcmin-2) Sstacked/Sinput

no bias

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Near-Infrared Selected Sources at z~1.5

Take advantage of statistics Split catalog up into groups of Similar Galaxies

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➡Assumption is that galaxies with similar

physical properties — described by their

  • ptical SEDs — will have similar infrared

properties.

➡This is Key! Only works if this assumption

holds.

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The Measurement

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

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  • UKIDSS/UDS [2/3 deg2] /


COSMOS [1.6 deg2] uBVRizJHK + IRAC ch1234 K-band cut 23.4 / 24 AB 80,000 / 120,000 sources

  • Redshifts - EAZY (Brammer 2008)
  • Masses - FAST (Kriek 2009)
  • Colors - UVJ (Williams 2009)

V - Jrest U - Vrest

Separating Quiescent from Star-forming

Muzzin et al. (2013)

Catalogs

SIMSTACK: Measurement Data

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SLIDE 18

marco.viero@stanford.edu Lisbon Seminar — May 3 2016

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  • Spitzer/MIPS
  • 24, 70μm
  • Herschel/PACS
  • 100, 160μm
  • Herschel/SPIRE
  • 250, 350, 500μm
  • ASTE/AzTEC
  • 1100μm

Maps

UDS - 1.4 x 1.4 deg Cosmos - 1.8 x 1.8 deg

SIMSTACK: Measurement Data

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×C1 ×C2 ×CN

+ …+ + …

➜ ➜ ➜

M = 9.5-10 X Y 996 1009 55 1011 187 1010 501 1011 336 1012 127 1011 M = 10.5-11 X Y 345 1029 340 1029 517 1027 805 1031 805 1031 238 1032 359 1033 841 1034 M = 10-10.5 X Y 535 1026 345 1029 340 1029 517 1027 805 1031 805 1031

z=1.0 to 1.5

… … …

≈

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

SIMSTACK: Flux Densities (M,z)

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

SIMSTACK: Flux Densities (M,z)

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Flux Density [mJy]

Wavelength [μm]

Viero, Moncelsi, Quadri+ (2013) arXiv:1304.0446

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

stellar mass slices redshift slices SIMSTACK: SEDs

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

stellar mass slices redshift slices

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{

SIMSTACK: LIR(M,z)

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

CIB Breakdown

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~70% at SPIRE wavelengths

Split Sample by:

  • redshift
  • stellar mass

log(M/M⊙~10-11) i.e., M ≲ M* z = 0-2 @ < 200um z = >1 @ > 200um

ULIRGS LIRGS Normal

Viero, Moncelsi, Quadri et al. (2013) arXiv:1304.0446

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

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SIMSTACK: Beyond Colour

  • Full SED Categorization

➡map physical features to FIR flux

Split into layers

redshift flux density

SIMSTACK

wavelength

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

  • Instead of fitting for

flux densities at each wavelength (one at a time),

  • Fit for luminosities

(i.e., SEDS) to full set

  • f maps at once

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SEDSTACK: Beyond Flux

nuInu log(wavelength) 500μm 350μm 250μm 160μm 100μm 1100μm

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

SEDSTACK in z - M - QT/SF bins

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  • Advantages:

➡leverage high

S/N components to better constrain faint-end

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

PEP — Magnelli 2013

  • SEDSTACK lets

us explore more layers (e.g, here 25)

  • Deeper than

“The deepest Herschel-PACS far-infrared survey” Magnelli (2013)

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SEDSTACK: Beyond Flux

Star-Forming Quiescent AGN Starburst Local

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SLIDE 29

So, 70% of CIB identified… what about the rest?

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SLIDE 30

marco.viero@stanford.edu Lisbon Seminar — May 3 2016

Aside: Correlated vs. Uncorrelated Emission

  • Uncorrelated

emission does not bias result,

  • nly increases

noise

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10,000 iterations

no bias

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SLIDE 31

marco.viero@stanford.edu Lisbon Seminar — May 3 2016

A New Accounting of the CIB

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Source in Catalog Source not in Catalog Imagine this is a SKY MAP

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

A New Accounting of the CIB

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Source in Catalog Source not in Catalog

Unbiased if :

  • beam is small

make synthetic “hits” map from positions of sources in catalog fit “synthetic” map to the map of the sky

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

A New Accounting of the CIB

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Source in Catalog Source not in Catalog

make synthetic “hits” map from positions of sources in catalog fit “synthetic” map to the map of the sky Biased if :

  • beam is big
  • missing a lot of sources
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SLIDE 34

marco.viero@stanford.edu Lisbon Seminar — May 3 2016

Viero, Moncelsi, Quadri et al. (2015) arXiv:1505.06242

A New Accounting of the CIB

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Smooth with bigger beam

COBE: Fixsen 1998 NULL TESTS

  • x-axis increasing beam
  • y-axis cumulative Intensity below z
  • FIRAS Direct measurement ~30% errors
  • Null tests on random positions
  • Flat because Catalog is ~100% complete

to log(M/Msun) = 9 - 11.5

  • Nearly all of the CIB is accounted for by

emission correlated with known, cataloged, galaxies. But is it necessarily

  • riginating from galaxies?
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SLIDE 35

marco.viero@stanford.edu Lisbon Seminar — May 3 2016

A New Accounting of the CIB

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  • Parametric fit to the (nominally) stacked flux densities (dashed lines)
  • Parametric fit to the stellar mass functions from Leja et al. 2014 (solid lines)

Stellar Mass Functions Submillimeter Flux Densities

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

A New Accounting of the CIB

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  • Circles/Solid lines: Model compared to total CIB after smoothing to 300

arcsec FWHM.

arcsec

Viero, Moncelsi, Quadri et al. (2015) arXiv:1505.06242

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

A New Accounting of the CIB: Summary

  • Current Estimates of the total CIB can be explained by known

galaxies, and their correlated companions, at z < 4

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  • This technique is

not limited to submillimeter maps

  • r CIB studies

➡as we push to

higher redshifts, intensities will be powerful probes of first galaxies, which will be faint, numerous, and highly correlated

Viero, Moncelsi et al. (2015) — arXiv:1505.06242

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

SIMSTACK: coming full circle

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Viero, Moncelsi, Quadri et al. (2013) arXiv:1304.0446

Flux RA DEC 41.4 149.853 2.608 3.5 149.854 2.258 4.4 149.752 2.584 16.7 149.832 2.724 22.5 149.275 2.196 3.6 149.262 2.966 5.8 149.915 2.206 3.1 149.546 2.564 2.3 149.824 2.047 4.0 149.453 2.278 2.1 149.863 2.788 … … …

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SLIDE 39

marco.viero@stanford.edu Lisbon Seminar — May 3 2016

SIMSTACK: coming full circle

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Flux RA DEC 41.4 149.853 2.608 3.5 149.854 2.258 4.4 149.752 2.584 16.7 149.832 2.724 22.5 149.275 2.196 3.6 149.262 2.966 5.8 149.915 2.206 3.1 149.546 2.564 2.3 149.824 2.047 4.0 149.453 2.278 2.1 149.863 2.788 … … …

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SLIDE 40

marco.viero@stanford.edu Lisbon Seminar — May 3 2016

PI: Viero

HerS HeLMS

HETDEX ACT SHELA SpIES

45°

350 deg2

SDSS Stripe 82

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  • HerS - 70 deg2 (~20 deg along S82)
  • HeLMS - 280 deg2 (~25 deg along S82)

SANEPIC maps made by Viktoria Asboth (UBC) and the SMAP team.

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HerS HeLMS

Find Maps/Catalogs at:

Viero+ 2014 arXiv:1308.4399 HerS: http://www.astro.caltech.edu/hers Oliver+ 2012 arXiv:1203.2562 HeLMS: http://hedam.lam.fr/HerMES/

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marco.viero@stanford.edu Lisbon Seminar — May 3 2016

Summary

  • Intensities are the way of the future, and not limited to FIR

➡as we push to higher redshifts, intensities will be powerful probes of

galaxies that are faint, numerous, and highly correlated

  • SIMSTACK/SEDSTACK works

➡Splitting up of sample needs improving, but eventually will ideally:

  • map optical/NIR features into infrared emission
  • explain the scatter in the star-forming “main sequence”
  • identify true outliers
  • provide measurement-based guidance for IR galaxy models
  • clean foregrounds for very high-z work

➡Python Code — https://github.com/marcoviero/simstack

  • Large SPIRE surveys in the SDSS Stripe 82 publicly available:

➡www.astro.caltech.edu/hers ➡hedam.lam.fr/HerMES/

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