High Redshift

Folkert Nobels

Kapteyn Astronomical Institute

June 8, 2017

Outline

Introduction

Population properties

Gravitational Lensed

High z surveys

I High z is z > 3.

I HDF (1995), HDF-S (1998),GOODS (2001-2002) HUDF(2004-2009), XDF (2012)

I HST, Spitzer, Chandra,XMM Newton

I WSRT, MERLIN, VLBI,ALMA

Types of galaxies

I Lyman-break galaxies (LBG)

I Lyman α emitter (LAE)

I Example spectra (z = 5.7)

[Dunlop, 2013]

Determination of redshift

I Photometric techniques:I Color selection

I SED FittingI Photometric redshift

I Spectroscopic TechniquesI Spectroscopic redshift

BoRG survey [Bradley et al., 2012],the HUDF09 program[McLure et al., 2010,Oesch et al., 2010,Bouwens et al., 2011], combinations[Bouwens et al., 2015]No K-band because of Thermalemission [STScI, 2017]

[Oesch et al., 2013]

Determination of redshift

I Photometric techniques:I Color selectionI SED FittingI Photometric redshift

I Spectroscopic TechniquesI Spectroscopic redshift

Synthetic models[Bruzual and Charlot, 2003],CANDELS and HUDF09 [Finkelsteinet al. 2010 and 2012], other fields[Mclure et al. 2009, 2010 and 2011]Photometric redshift

[McLure et al., 2010]

Determination of redshift

I Photometric techniques:I Color selectionI SED FittingI Photometric redshift

I Spectroscopic TechniquesI Spectroscopic redshift

Weak lensing surveys: Subaru[Hamana et al., 2009]BAO and ELG: BigBOSS[Schlegel et al., 2011]Deep Surveys: VLT and MUSE[Garel et al., 2016]Determining Dynamical properties:KMOS [Stott et al., 2016]

[Ouchi et al., 2008]

Lyman Alpha and comparison of redshift methods

I Lyman alpha profiles areabsorbed

I Accuracy of spectroscopicredshift vs photometricredshift

[Erb et al., 2016]

Lyman Alpha and comparison of redshift methods

I Lyman alpha profiles areabsorbed

I Accuracy of spectroscopicredshift vs photometricredshift

[Fernandez-Soto et al., 2001]

Halo Mass Function (HMF)

I Press-Schechter HMF

I Sheth-Tormen HMFI Fitting N-body

simulationsI Biased

108 109 1010 1011 1012 1013

M/M¯

10-10

10-9

10-8

10-7

10-6

10-5

10-4

10-3

10-2

10-1

100

101

102

dn

dlo

g 10M

The Press-Schechter HMF

z=4

z=5

z=6

z=7

z=8

z=9

z=10

z=11

z=12

z=13

z=14

z=15

http://hmf.icrar.org/

Halo Mass Function (HMF)

I Press-Schechter HMFI Sheth-Tormen HMF

I Fitting N-bodysimulations

I Biased 108 109 1010 1011 1012 1013

M/M¯

10-10

10-9

10-8

10-7

10-6

10-5

10-4

10-3

10-2

10-1

100

101

102

dn

dlo

g 10M

The Sheth-Tormen HMF

z=4

z=5

z=6

z=7

z=8

z=9

z=10

z=11

z=12

z=13

z=14

z=15

http://hmf.icrar.org/

UV Luminosity Function (UVLF)

I number of galaxies permagnitude bin

I φ(L)dL = dndLdL =

φ?(LL?

)αe−

LL? d

(LL?

)

I Declining with redshift

[Bouwens et al., 2015]

UV Luminosity Function (UVLF)

I number of galaxies permagnitude bin

I φ(L)dL = dndLdL =

φ?(LL?

)αe−

LL? d

(LL?

)I Declining with redshift

[Bouwens et al., 2015]

Specific Star Formation Rate (sSFR)

I SFR over mass

I Assume a MUV -M? relation.

I Or use sophisticated modelesophisticated model

[Faisst et al., 2016]

Stellar Mass Density (SMD)

I Density of stellar mass atspecific redshifts

I Spitzer

[Stark et al., 2013]

Stellar Mass Density (SMD)

I Density of stellar mass atspecific redshifts

I Spitzer

[Song et al., 2016]

Stellar Mass Function (SMF)

I Number of galaxies perstellar mass

[Song et al., 2016]

Mass/Light ratio

I M/L for galaxies

[Song et al., 2016]

Gravitational Lensed

I Advantage:I Boost total fluxI efficient for unresolved

sourcesI multiple images

I Disadvantage:I Effective area smallerI Estimate of magnification

[Smail et al., 2007]

Gravitational Lensed: Individual

I HST and Keck

I For ground galaxy atz = 0.73

I Galaxy cluster at z = 0.33

I LBG spectrum

I Magnification 28± 3

I 100 parsecs resolution

I Determine internal dynamics

I Derived from [OIII] line

I Rotation curve

[Smail et al., 2007]

Gravitational Lensed: Individual

I HST and Keck

I For ground galaxy atz = 0.73

I Galaxy cluster at z = 0.33

I LBG spectrum

I Magnification 28± 3

I 100 parsecs resolution

I Determine internal dynamics

I Derived from [OIII] line

I Rotation curve

[Stark et al., 2008]

Gravitational Lensed: Individual

I HST and Keck

I For ground galaxy atz = 0.73

I Galaxy cluster at z = 0.33

I LBG spectrum

I Magnification 28± 3

I 100 parsecs resolution

I Determine internal dynamics

I Derived from [OIII] line

I Rotation curve

[Stark et al., 2008]

Gravitational Lensed: population

I Lensing model

I z ≈ 6, 7, 8, and9 areindicated by green, cyan,magenta, and yellow circles.

I magnification: > 50

I Redshift probabilitydistribution

I State-of-the-art UVLF

[Livermore et al., 2017]

Gravitational Lensed: population

I Lensing model

I z ≈ 6, 7, 8, and9 areindicated by green, cyan,magenta, and yellow circles.

I magnification: > 50

I Redshift probabilitydistribution

I State-of-the-art UVLF

[Livermore et al., 2017]

Gravitational Lensed: population

I Lensing model

I z ≈ 6, 7, 8, and9 areindicated by green, cyan,magenta, and yellow circles.

I magnification: > 50

I Redshift probabilitydistribution

I State-of-the-art UVLF

[Livermore et al., 2017]

Gravitational Lensed: population

I High redshift with photometry or spectroscopy

I Different population measurements: HMF, UVLF, sSFR,SMD, SMF, M/L-ratio.

I Gravitational lensing could be used on 1 target or to inferpopulation properties

References I

Bouwens, R. J., Illingworth, G. D., Oesch, P. A., Labbe, I., Trenti, M., van Dokkum, P., Franx, M., Stiavelli,

M., Carollo, C. M., Magee, D., and Gonzalez, V. (2011).Ultraviolet Luminosity Functions from 132 z ∼ 7 and z ∼ 8 Lyman-break Galaxies in the Ultra-deepHUDF09 and Wide-area Early Release Science WFC3/IR Observations.The Astrophysical Journal, 737:90.

Bouwens, R. J., Illingworth, G. D., Oesch, P. A., Trenti, M., Labbe, I., Bradley, L., Carollo, M., van

Dokkum, P. G., Gonzalez, V., Holwerda, B., Franx, M., Spitler, L., Smit, R., and Magee, D. (2015).UV Luminosity Functions at Redshifts z ∼ 4 to z ∼ 10: 10,000 Galaxies from HST Legacy Fields.The Astrophysical Journal, 803:34.

Bradley, L. D., Trenti, M., Oesch, P. A., Stiavelli, M., Treu, T., Bouwens, R. J., Shull, J. M., Holwerda,

B. W., and Pirzkal, N. (2012).The Brightest of Reionizing Galaxies Survey: Constraints on the Bright End of the z ˜ 8 LuminosityFunction.The Astrophysical Journal, 760:108.

Bruzual, G. and Charlot, S. (2003).

Stellar population synthesis at the resolution of 2003.Monthly Notice of the Royal Astronomical Society, 344:1000–1028.

Dunlop, J. S. (2013).

Observing the First Galaxies.In Wiklind, T., Mobasher, B., and Bromm, V., editors, The First Galaxies, volume 396 of Astrophysics andSpace Science Library, page 223.

Erb, D. K., Pettini, M., Steidel, C. C., Strom, A. L., Rudie, G. C., Trainor, R. F., Shapley, A. E., and

Reddy, N. A. (2016).A High Fraction of Lyα Emitters among Galaxies with Extreme Emission Line Ratios at z ˜2.Astrophysical Journal, 830:52.

References II

Faisst, A. L., Capak, P., Hsieh, B. C., Laigle, C., Salvato, M., Tasca, L., Cassata, P., Davidzon, I., Ilbert,

O., Le Fevre, O., Masters, D., McCracken, H. J., Steinhardt, C., Silverman, J. D., de Barros, S., Hasinger,G., and Scoville, N. Z. (2016).A Coherent Study of Emission Lines from Broadband Photometry: Specific Star Formation Rates and [Oiii]/Hβ Ratio at 3 < z < 6.The Astrophysical Journal, 821:122.

Fernandez-Soto, A., Lanzetta, K. M., Chen, H.-W., Pascarelle, S. M., and Yahata, N. (2001).

On the Compared Accuracy and Reliability of Spectroscopic and Photometric Redshift Measurements.Astrophysical Journal, Supplements, 135:41–61.

Finkelstein, S. L., Papovich, C., Giavalisco, M., Reddy, N. A., Ferguson, H. C., Koekemoer, A. M., and

Dickinson, M. (2010).On the Stellar Populations and Evolution of Star-forming Galaxies at 6.3 < z <= 8.6.Astrophysical Journal, 719:1250–1273.

Finkelstein, S. L., Papovich, C., Salmon, B., Finlator, K., Dickinson, M., Ferguson, H. C., Giavalisco, M.,

Koekemoer, A. M., Reddy, N. A., Bassett, R., Conselice, C. J., Dunlop, J. S., Faber, S. M., Grogin, N. A.,Hathi, N. P., Kocevski, D. D., Lai, K., Lee, K.-S., McLure, R. J., Mobasher, B., and Newman, J. A. (2012).Candels: The Evolution of Galaxy Rest-frame Ultraviolet Colors from z = 8 to 4.Astrophysical Journal, 756:164.

Garel, T., Guiderdoni, B., and Blaizot, J. (2016).

Lyman-α emitters in the context of hierarchical galaxy formation: predictions for VLT/MUSE surveys.Monthly Notice of the Royal Astronomical Society, 455:3436–3452.

Hamana, T., Miyazaki, S., Kashikawa, N., Ellis, R. S., Massey, R. J., Refregier, A., and Taylor, J. E. (2009).

Subaru Weak-Lensing Survey II: Multi-Object Spectroscopy and Cluster Masses.Publications of the ASJ, 61:833–872.

References III

Livermore, R. C., Finkelstein, S. L., and Lotz, J. M. (2017).

Directly Observing the Galaxies Likely Responsible for Reionization.Astrophysical Journal, 835:113.

McLure, R. J., Cirasuolo, M., Dunlop, J. S., Foucaud, S., and Almaini, O. (2009).

The luminosity function, halo masses and stellar masses of luminous Lyman-break galaxies at redshifts 5 <z < 6.Monthly Notice of the Royal Astronomical Society, 395:2196–2209.

McLure, R. J., Dunlop, J. S., Cirasuolo, M., Koekemoer, A. M., Sabbi, E., Stark, D. P., Targett, T. A., and

Ellis, R. S. (2010).Galaxies at z = 6-9 from the WFC3/IR imaging of the Hubble Ultra Deep Field.Monthly Notice of the Royal Astronomical Society, 403:960–983.

McLure, R. J., Dunlop, J. S., de Ravel, L., Cirasuolo, M., Ellis, R. S., Schenker, M., Robertson, B. E.,

Koekemoer, A. M., Stark, D. P., and Bowler, R. A. A. (2011).A robust sample of galaxies at redshifts 6.0<z<8.7: stellar populations, star formation rates and stellarmasses.Monthly Notice of the Royal Astronomical Society, 418:2074–2105.

Oesch, P. A., Bouwens, R. J., Illingworth, G. D., Carollo, C. M., Franx, M., Labbe, I., Magee, D., Stiavelli,

M., Trenti, M., and van Dokkum, P. G. (2010).z ˜ 7 Galaxies in the HUDF: First Epoch WFC3/IR Results.Astrophysical Journal, Letters, 709:L16–L20.

Oesch, P. A., Bouwens, R. J., Illingworth, G. D., Labbe, I., Franx, M., van Dokkum, P. G., Trenti, M.,

Stiavelli, M., Gonzalez, V., and Magee, D. (2013).Probing the Dawn of Galaxies at z ˜ 9-12: New Constraints from HUDF12/XDF and CANDELS data.Astrophysical Journal, 773:75.

References IV

Ouchi, M., Shimasaku, K., Akiyama, M., Simpson, C., Saito, T., Ueda, Y., Furusawa, H., Sekiguchi, K.,

Yamada, T., Kodama, T., Kashikawa, N., Okamura, S., Iye, M., Takata, T., Yoshida, M., and Yoshida, M.(2008).The Subaru/XMM-Newton Deep Survey (SXDS). IV. Evolution of Lyα Emitters from z = 3.1 to 5.7 in the

1 deg2 Field: Luminosity Functions and AGN.Astrophysical Journal, Supplements, 176:301–330.

Schlegel, D., Abdalla, F., Abraham, T., Ahn, C., Allende Prieto, C., Annis, J., Aubourg, E., Azzaro, M.,

Baltay, S. B. C., Baugh, C., Bebek, C., Becerril, S., Blanton, M., Bolton, A., Bromley, B., Cahn, R.,Carton, P. ., Cervantes-Cota, J. L., Chu, Y., Cortes, M., Dawson, K., Dey, A., Dickinson, M., Diehl, H. T.,Doel, P., Ealet, A., Edelstein, J., Eppelle, D., Escoffier, S., Evrard, A., Faccioli, L., Frenk, C., Geha, M.,Gerdes, D., Gondolo, P., Gonzalez-Arroyo, A., Grossan, B., Heckman, T., Heetderks, H., Ho, S., Honscheid,K., Huterer, D., Ilbert, O., Ivans, I., Jelinsky, P., Jing, Y., Joyce, D., Kennedy, R., Kent, S., Kieda, D., Kim,A., Kim, C., Kneib, J. ., Kong, X., Kosowsky, A., Krishnan, K., Lahav, O., Lampton, M., LeBohec, S., LeBrun, V., Levi, M., Li, C., Liang, M., Lim, H., Lin, W., Linder, E., Lorenzon, W., de la Macorra, A.,Magneville, C., Malina, R., Marinoni, C., Martinez, V., Majewski, S., Matheson, T., McCloskey, R.,McDonald, P., McKay, T., McMahon, J., Menard, B., Miralda-Escude, J., Modjaz, M., Montero-Dorta, A.,Morales, I., Mostek, N., Newman, J., Nichol, R., Nugent, P., Olsen, K., Padmanabhan, N.,Palanque-Delabrouille, N., Park, I., Peacock, J., Percival, W., Perlmutter, S., Peroux, C., Petitjean, P.,Prada, F., Prieto, E., Prochaska, J., Reil, K., Rockosi, C., Roe, N., Rollinde, E., Roodman, A., Ross, N.,Rudnick, G., Ruhlmann-Kleider, V., Sanchez, J., Sawyer, D., Schimd, C., Schubnell, M., Scoccimaro, R.,Seljak, U., Seo, H., Sheldon, E., Sholl, M., Shulte-Ladbeck, R., Slosar, A., Smith, D. S., Smoot, G.,Springer, W., Stril, A., Szalay, A. S., Tao, C., Tarle, G., Taylor, E., Tilquin, A., Tinker, J., Valdes, F.,Wang, J., Wang, T., Weaver, B. A., Weinberg, D., White, M., Wood-Vasey, M., Yang, J., Yeche, X. Y. C.,Zakamska, N., Zentner, A., Zhai, C., and Zhang, P. (2011).The BigBOSS Experiment.ArXiv e-prints.

References V

Smail, I., Swinbank, A. M., Richard, J., Ebeling, H., Kneib, J.-P., Edge, A. C., Stark, D., Ellis, R. S., Dye,

S., Smith, G. P., and Mullis, C. (2007).A Very Bright, Highly Magnified Lyman Break Galaxy at z = 3.07.Astrophysical Journal, Letters, 654:L33–L36.

Song, M., Finkelstein, S. L., Ashby, M. L. N., Grazian, A., Lu, Y., Papovich, C., Salmon, B., Somerville,

R. S., Dickinson, M., Duncan, K., Faber, S. M., Fazio, G. G., Ferguson, H. C., Fontana, A., Guo, Y., Hathi,N., Lee, S.-K., Merlin, E., and Willner, S. P. (2016).The Evolution of the Galaxy Stellar Mass Function at z = 4-8: A Steepening Low-mass-end Slope withIncreasing Redshift.The Astrophysical Journal, 825:5.

Stark, D. P., Schenker, M. A., Ellis, R., Robertson, B., McLure, R., and Dunlop, J. (2013).

Keck Spectroscopy of 3 ≤ z ≤ 7 Faint Lyman Break Galaxies: The Importance of Nebular Emission inUnderstanding the Specific Star Formation Rate and Stellar Mass Density.The Astrophysical Journal, 763:129.

Stark, D. P., Swinbank, A. M., Ellis, R. S., Dye, S., Smail, I. R., and Richard, J. (2008).

The formation and assembly of a typical star-forming galaxy at redshift z˜3.Nature, 455:775–777.

Stott, J. P., Swinbank, A. M., Johnson, H. L., Tiley, A., Magdis, G., Bower, R., Bunker, A. J., Bureau, M.,

Harrison, C. M., Jarvis, M. J., Sharples, R., Smail, I., Sobral, D., Best, P., and Cirasuolo, M. (2016).The KMOS Redshift One Spectroscopic Survey (KROSS): dynamical properties, gas and dark matterfractions of typical z ∼ 1 star-forming galaxies.Monthly Notice of the Royal Astronomical Society, 457:1888–1904.

STScI (2017).

NICMOS: The Infrared Background.