Clumpy galaxies at high redshift: Insights from the NIHAO - PowerPoint PPT Presentation

Clumpy galaxies at high redshift: Insights from the NIHAO simulations Buck et al. 2017 (MNRAS) - arXiv:1612.05277 Gas in Galaxies Valetta 6th of October Tobias Buck Andrea V. Macciò, Aura Obreja, Aaron A. Dutton, Hans-Walter Rix PhD student at MPIA

Intro: What are clumpy galaxies? • star forming disc galaxies at redshift 0.5 - 3 • observed to have UV-bright / H-alpha-bright clumps • clump sizes ~1 kpc, clump masses 1e8 - 1e10 Msun simulation Gas in Galaxies, Valetta Tobias Buck 2 06.10.17

Intro: Clumpy galaxies in observations Elmegree+2013 Guo+2015 Wuyts+2012 Gas in Galaxies, Valetta Tobias Buck 3 06.10.17

Why are clumpy galaxies interesting previous works/simulations • clump formation via V iolent D isc I nstability (Dekel+2009) • color gradient: clump inspiral 540 Myr 760 Myr Bournaud+2014 Gas surface density Obs.: Genzel+2006,2009, Förster-Schreiber+2006,2011, Wuyts+2012, Elmegreen+2013, Tadaki+2014, Murata+2014, Guo+2015, simulation Shibuya+2016 Theory: Bournaud+2007,2008,2009,2014, Dekel+2009, Ceverino+2010,2012, Mandelker+2014, Moody+2014, Tamburello+2015, Mayer+2016, Oklopcic+2017 Gas in Galaxies, Valetta Tobias Buck 4 06.10.17

Why are clumpy galaxies interesting previous works/simulations • clump formation via V iolent D isc I nstability (Dekel+2009) • color gradient: clump inspiral 540 Myr 760 Myr Bournaud+2014 Gas surface density Obs.: Genzel+2006,2009, Förster-Schreiber+2006,2011, Wuyts+2012, Elmegreen+2013, Tadaki+2014, Murata+2014, Guo+2015, simulation Shibuya+2016 Theory: Bournaud+2007,2008,2009,2014, Dekel+2009, Ceverino+2010,2012, Mandelker+2014, Moody+2014, Tamburello+2015, Mayer+2016, Oklopcic+2017 Gas in Galaxies, Valetta Tobias Buck 4 06.10.17

Why are clumpy galaxies interesting previous works/simulations • clump formation via V iolent D isc I nstability (Dekel+2009) • color gradient: clump inspiral Genel+2012 winds Gas surface density 540 Myr 760 Myr 4kpc ] Mass [M Bournaud+2014 Gas surface density z=2.03, t=22Myr z=2.012, t=52Myr z=2.021, t=37Myr Obs.: Genzel+2006,2009, Förster-Schreiber+2006,2011, Wuyts+2012, Elmegreen+2013, Tadaki+2014, Murata+2014, Guo+2015, simulation Shibuya+2016 Theory: Bournaud+2007,2008,2009,2014, Dekel+2009, Ceverino+2010,2012, Mandelker+2014, Moody+2014, Tamburello+2015, Mayer+2016, Oklopcic+2017 Gas in Galaxies, Valetta Tobias Buck 4 06.10.17

Observed vs. simulated clumps: some tension… simulations disagree on fate of clumps simulations and observations probe di ff erent things - observations: clumps in stellar light - most theory: clumps in gas density ? = light gas simulation Bournaud+2014 Guo+2015 Gas in Galaxies, Valetta Tobias Buck 5 06.10.17

The NIHAO Simulation suite 90 zoom-in simulations from Milky-Way mass to dwarf galaxies scales NIHAO I: Wang+15 (82 galaxies in this plots) g8.26e11 Gas in Galaxies, Valetta Tobias Buck 6 06.10.17

The NIHAO Simulation suite 90 zoom-in simulations from Milky-Way mass to dwarf galaxies scales NIHAO I: Wang+15 (82 galaxies in this plots) g8.26e11 Gas in Galaxies, Valetta Tobias Buck 6 06.10.17

The post processing of NIHAO 19 high mass galaxies from the NIHAO sample M_star > 1e9 M_sun at redshift z=1.5 Selection of clumps in light „intrinsic“ Gas in Galaxies, Valetta Tobias Buck 7 06.10.17

The post processing of NIHAO 19 high mass galaxies from the NIHAO sample M_star > 1e9 M_sun at redshift z=1.5 Selection of clumps in light A. intrinsic luminosity calculated from simple stellar populations „intrinsic“ „intrinsic“ Gas in Galaxies, Valetta Tobias Buck 7 06.10.17

The post processing of NIHAO 19 high mass galaxies from the NIHAO sample M_star > 1e9 M_sun at redshift z=1.5 Selection of clumps in light A. intrinsic luminosity calculated from simple stellar populations „intrinsic“ „intrinsic“ B. radiative transfer post processing with GRASIL-3D (Domìnguez-Tenreiro+2014) „observed“ Gas in Galaxies, Valetta Tobias Buck 7 06.10.17

The „observed“ clumpy fraction of NIHAO Fraction of galaxies with clumps Gas in Galaxies, Valetta Tobias Buck 8 06.10.17

The „observed“ clumpy fraction of NIHAO Fraction of galaxies with clumps Gas in Galaxies, Valetta Tobias Buck 9 06.10.17

The „observed“ clumpy fraction of NIHAO Fraction of galaxies with clumps Gas in Galaxies, Valetta Tobias Buck 9 06.10.17

The „observed“ clumpy fraction of NIHAO Fraction of galaxies with clumps Gas in Galaxies, Valetta Tobias Buck 9 06.10.17

The „intrinsic“ clumps of NIHAO Gas U-Band U-Band Stars SFR Gas in Galaxies, Valetta Tobias Buck 10 06.10.17

The „intrinsic“ clumps of NIHAO Gas U-Band U-Band Stars SFR Gas in Galaxies, Valetta Tobias Buck 10 06.10.17

The „intrinsic“ clumps of NIHAO Gas U-Band U-Band Stars SFR Gas in Galaxies, Valetta Tobias Buck 10 06.10.17

The „intrinsic“ clumps of NIHAO Gas U-Band U-Band Stars SFR Gas in Galaxies, Valetta Tobias Buck 10 06.10.17

The „intrinsic“ clumps of NIHAO Gas U-Band U-Band Stars SFR Gas in Galaxies, Valetta Tobias Buck 10 06.10.17

The „intrinsic“ clumps of NIHAO Number of clumps per snapshot Number of clumps per snapshot Gas in Galaxies, Valetta Tobias Buck 11 06.10.17

The „intrinsic“ clumps of NIHAO Number of clumps per snapshot Gas in Galaxies, Valetta Tobias Buck 11 06.10.17

The „intrinsic“ clumps of NIHAO Number of clumps per snapshot NO clumps in stars Gas in Galaxies, Valetta Tobias Buck 11 06.10.17

Stellar mass maps of observations Wuyts+2012 NB209-7 V 606 M * I V 606 M * I NB209-12 Gas in Galaxies, Valetta Tobias Buck 12 06.10.17

Stellar mass maps of observations Wuyts+2012 NB209-7 V 606 M * I V 606 M * I NB209-12 RGB U-Band stellar mass Gas in Galaxies, Valetta Tobias Buck 12 06.10.17

Conclusions Clumpy galaxies in NIHAO: • agree well with observed relations • are ONLY present in stellar light • can NOT be found in stellar mass • are not long lived and do not contribute to bulge growth Gas in Galaxies, Valetta Tobias Buck 13 06.10.17

RGB composite Conclusions Clumpy galaxies in NIHAO: • agree well with observed relations U-Luminosity • are ONLY present in stellar light • can NOT be found in stellar mass • are not long lived and do not contribute to bulge growth TB+2017 Gas in Galaxies, Valetta Tobias Buck 13 06.10.17

Extra Material Ut wisi enim ad minim veniam, quis nostrud exerci tation ullamcorper suscipit lobortis nisl ut aliquip ex ea commodo consequat. Duis autem vel eum iriure dolor in hendrerit in vulputate velit esse molestie consequat, vel illum 14

The „intrinsic“ clumps of NIHAO Gas in Galaxies, Valetta Tobias Buck 15 06.10.17

The „intrinsic“ clumps of NIHAO Gas in Galaxies, Valetta Tobias Buck 16 06.10.17

Differences to other Simulations 10 � 3 FIRE VELA Inoue15 MIRAGE VELA RP 0 . 4 VELA NIHAO 10 � 1 M ? /M 200 0 . 2 10 � 2 z=2 10 � 3 0 . 0 10 9 10 10 10 11 10 12 0 . 0 0 . 2 0 . 4 10 10 0 . 4 10 M [M M 200 [M � ] Tobias Buck MPIA Galaxy Coffee 17 06.10.17

Differences to other Simulations Rad. Press. no Rad Press. Tobias Buck MPIA Galaxy Coffee 17 06.10.17

Differences to other Simulations Feedback prescription is crucial Rad. Press. no Rad Press. for clump formation/survival Tobias Buck MPIA Galaxy Coffee 17 06.10.17

The fate of „intrinsic“ clumps in NIHAO Gas in Galaxies, Valetta Tobias Buck 18 06.10.17

The „observed“ clumpy fraction of NIHAO - correlation with galaxy property Gas in Galaxies, Valetta Tobias Buck 19 06.10.17

The „observed“ clumpy fraction of NIHAO - correlation with galaxy property „compactness“ Gas in Galaxies, Valetta Tobias Buck 19 06.10.17

The „observed“ clump properties of NIHAO fractional UV light contribution 10 − 1 F¨ orster-Schreiber+2011 NIHAO 1.0 1.5 2.0 Gas in Galaxies, Valetta Tobias Buck 20 06.10.17

The Gas fraction of NIHAO 1 . 0 NIHAO z=0 z=0 z=1 MIRAGE 0 . 8 z=0 (Dutton+11) f gas = M gas / ( M gas +M ? ) 0 . 6 NIHAO z=1 0 . 4 VELA MIRAGE FIRE m13 0 . 2 PHIBSS corr PHIBBS 0 . 0 10 9 10 10 10 11 10 9 10 10 10 11 M ? [M � ] M ? [M � ] Gas in Galaxies, Valetta Tobias Buck 21 06.10.17