CITA Extragalactic Sims: Current Snapshot

Transcription

1 CITA Extragalactic Sims: Current Snapshot Low-z Clusters & Groups 320 realizations (M > 2 x Msun/h, z < 1.25) High-z Clusters & Groups + Subgrid Biasing Single realization (M > 2 x Msun/h, z < 4.5) Alvarez, Bond, Stein Bahmanyar, Battaglia, Pham, van Engelen Halo Catalogs: [x, y, z, vx, vy, vz, Mvir] Maps: [tsz, ksz, κcmb, CIB] questions/requests: malvarez@cita.utoronto.ca Mapmaking pipeline SZ, CIB, lensing Alvarez et al. (2017) Input: profile table, halo catalog, unlensed primary Output: lensed CMB, SZ, CIB Battaglia et al. (2012) + = halo catalog and/or linear density tabulated profile and/or bias parameters multifrequency maps

2 CITA SZ/CIB Sims Alvarez, Bond, Stein, Battaglia Systematics & foregrounds 1. Baryonic physics effects on halo mass 2. tsz - CIB (important for ksz power) 3. Cosmic variance at low z and high Mhalo 4. External data set calibration 5. Scatter/anisotropy in mass-observable * bullets increase with z at fixed M 6. Neutrino effects on halo mass * beyond linear + LCDM hmf 7. Velocity bias of halos (for ksz cf RSD) Currently being addressed 1. Spherical gas/stars/pressure/dm profiles from a single sim (Battaglia et al.) 2. Planck model for CIB x tsz 3. Large ensembles * ~500 Mhalo > 2e13 and z<1.3 done 4. CMASS HOD mocks Science Requirements 1. Σm ν / σ 8 (z) / w(z) 2. fσ 8 (z) 3. Δz reion / τ es 4. (P, ρ) vs (M halo, z) Going forward (priorities?) 1. More realistic halo model * correlate with substructure and tides 2. Scan astrophysical parameter space * hydro sim calibration (eg CCA galform) * couple to external obs (eg CCAT-p) 3. External structure * the cosmic web * missing baryons 4. Beyond LCDM * neutrinos, modified gravity 5. Correlated external data set mocks * LSST, HIRAX, Euclid, WFIRST, 6. Reionization ksz/tsz 7. Integration into end-to-end data analysis pipeline for validation

3 CITA Lensing Sims Alvarez, Stein, Bond, van Engelen, Battaglia, Codis, Liu Systematics & foregrounds 1. Baryonic physics effects on mass dist. 2. CIB non-gaussianity & lensing reconst. 3. External data set calibration 4. Scatter/anisotropy in mass-observable * bullets increase with z at fixed M 5. Neutrino effects on halo mass * beyond linear + LCDM hmf 6.??? Currently being addressed 1. Spherical gas/stars/dm profiles from a single sim (Battaglia et al.) 2. Planck model for CIB x tsz 3. Lensing of primary with Borne 4. Comparing LPT for matter outside halos to N-body 5. CMASS HOD mocks Science Requirements 1. r 2. Σm ν / σ 8 (z) / w(z) 3. ρ vs (M halo, z) Going forward (priorities?) 1. More realistic halo model * correlate with substructure and tides 2. Scan astrophysical parameter space * hydro sim calibration (eg CCA galform) * couple to external obs (eg Herschel) 3. External structure * the cosmic web * missing baryons 4. Beyond LCDM * neutrinos, modified gravity 5. Correlated external data set mocks * LSST, HIRAX, Euclid, WFIRST, 6. Integration into end-to-end data analysis pipeline for validation

4 CITA Lensing Sims Alvarez, Stein, Bond, van Engelen, Battaglia, Codis, Liu

5 CITA Lensing Sims Alvarez, Stein, Bond, van Engelen, Battaglia, Codis, Liu

6 CITA Lensing Sims Alvarez, Stein, Bond, van Engelen, Battaglia, Codis, Liu

7 CITA Lensing Sims Alvarez, Stein, Bond, van Engelen, Battaglia, Codis, Liu

8 Point source and atmosphere effects on tsz science Kevin Huffenberger Florida State University

9 Setup Predict ILC-multifrequency reconstruction of Compton-y power spectrum. Fast... can run suites of instrument models. Multi-component sky model with tsz, ksz, CIB sources, Radio sources. Source flux cuts computed self-consistently.

10 l(l + 1)Cl/2π (µk 2 ) GHz cmb cibc cibp radp ksz multipole l

11 S 2.5 dn ds (sr 1 Jy 1 5 ) D3000 (μk 2 ) GHz Bethermin 2012, modified so total power is not too high CIB counts CIB power Conf. limits with "10m," "7m," "5m" Flux density S (mjy)

12 "7m" configuration channels (GHz) beam fwhm (arcmin) channel map noise (muk-arcmin) effective map noise = 2.25 muk-arcmin fsky = 0.50 optional atmosphere: cf Hasselfield

13 7.0 "7m" dish, flux cut vs. noise GHz flux cut (mjy) GHz noise (µk-arcmin)

14 l(l + 1)ClT 2 cmb /2π (µk2 ) strawso_2016octcaseb_5.0m_fsky50_5yr_drop270 err per multipole noise power tsz compton y multipole l

15 l(l + 1)ClT 2 cmb /2π (µk2 ) Compton y noise strawso_2016octcaseb_5.0m_fsky50_5yr err per multipole noise power tsz compton y multipole l

16 l(l + 1)ClT 2 cmb /2π (µk2 ) Compton y noise strawso_2016octcasec_7.0m_fsky50_5yr err per multipole noise power tsz compton y multipole l

17 l(l + 1)ClT 2 cmb /2π (µk2 ) strawso_2016octcasec_7.0m_fsky50_5yr_atmsimple err per multipole noise power tsz compton y multipole l

18 µk, 5.0 m, fsky = 50 w/ l knee = µk, 7.0 m, fsky = 50 w/ l knee = 3400 S/N( > lmin) minimum multipole l min

19 Are foregrounds important for ksz? 1 When overlapping with spectroscopy, the standard estimators are differential à most components that are uncorrelated with velocities average out as 1/ p N objects Turn bias into noise à may not need as good cleaning as for other science? But how big is the extra noise? And Can this fail in the high S/N regime? Yes, in a few ways! Cancellation can be imperfect for extreme objects (e.g. tsz) Extragalactic can also impose a similar noise floor à need to estimate! Foregrounds can be correlated with velocity Projected fields, power spectrum, 4pt function: foregrounds Simone Ferraro (Berkeley)

20 Atmospheric noise in T 2 Louis Simone Ferraro (Berkeley)

21 Effect of atmospheric noise 3 Optimistic scenario PRELIMINARY Simone Ferraro (Berkeley)

22 Adding foregrounds + atmosphere 4 ILC on foregrounds only with 5 frequency channels PRELIMINARY! ILC mitigation NO foregrounds/atm RAW foregrounds + atm Simone Ferraro (Berkeley)

23 Small Angular Scales Discussion Session: Clusters Lindsey Bleem CMB-S4 Workshop 2/28/17

24 Science Reach/Systematics/ Dependencies What can CMB clusters + LSST clusters do, how much better than S3+LSST? Do we need S4 to reach interesting depth or would more time with existing large aperture facilities (SPT, ACT) be enough? Catalog-based modeling underway; more sophisticated modeling longer term effort! Modeling selection (what is going on in the highest-z clusters? [not foregrounds per se]); false associations; incomplete follow-up (can we get all the telescope time we need to follow up high-z clusters?) Learning a lot from S1-S3 experiments; Telescope access open question! MASS CALIBRATION Optical Weak lensing systematics: shear bias, photo-zs, cluster member contamination, miscentering, profile assumptions Share problems with LSST cluster samples, simulation + data driven efforts underway to tackle these issues! CMB weak lensing biases: tsz, ksz, CIB+Synchrotron from cluster members Correlated Observables - Simulations, targeted followup observations Theoretical Mass Function -> Observed cluster relation (differences in halo catalogs, observer definition of clusters, etc)

25 Slide from Steve Allen s Talk The discovery space for CMB-S4 Primary discovery space

26 Science Reach/Systematics/ Dependencies What can CMB clusters + LSST clusters do, how much better than S3+LSST? Do we need S4 to reach interesting depth or would more time with existing large aperture facilities (SPT, ACT) be enough? Catalog-based modeling underway! Modeling selection (what is going on in the highest-z clusters? [not foregrounds per se]); false associations; incomplete follow-up (can we get all the telescope time we need to follow up high-z clusters?) Learning a lot from S1-S3 experiments; Telescope access open question! MASS CALIBRATION Optical Weak lensing systematics: shear bias, photo-zs, cluster member contamination, miscentering, profile assumptions Share problems with LSST cluster samples, simulation + data driven efforts underway to tackle these issues! CMB weak lensing biases: tsz, ksz, CIB+Synchrotron from cluster members Correlated Observables - Simulations, targeted followup observations Theoretical Mass Function -> Observed cluster relation (differences in halo catalogs, observer definition of clusters, etc)

27 Connecting Simulations to Observations: tsz + ksz: Baryons added in post processing. (Flender+16; ApJ 823, 98F) Forecasts pairwise ksz signal from DES+SPT; DESI+ACTpol Lensing Pipelines Weak Lensing (OpVcal + CMB) PICS: RealisVc Strong Lensing Pipeline (Li+2016; ApJ 828,1, 54) Galaxies in Simulated Clusters! A mul&-wavelength view of clusters in next genera&on surveys (SZ, Op&cal, X-ray) CMB-S4 Workshop, SLAC, 2/27/17 Simulated cluster tsz, weak- and strong-lensing signals 5

28 Connecting Simulations to Observations: tsz + ksz: Baryons added in post processing. (Flender+16; ApJ 823, 98F) Forecasts pairwise ksz signal from DES+SPT; DESI+ACTpol Key interprevng DES+SPT pairwise ksz signal (Soergel +2016;MNRAS S) Lensing Pipelines Weak Lensing (OpVcal + CMB) PICS: RealisVc Strong Lensing Pipeline (Li+2016; ApJ 828,1, 54) Galaxies in Simulated Clusters Galaxy Placement in halos [D. Korytov+ in prep] CMB-S4 Workshop, SLAC, 2/27/17 6

29 ExaSky: Conservative Conservatice Reproducing Reproducing Kernel Kernel SPH (Particle SPH (Particle Hydro) Hydro) Triple-point shock test with CRKSPH, Frontiere et al 2016 Frontiere, Raskin, Owen, J. Comp. Phys. (2017); arxiv: [physics.comp-ph] Blob test, Frontiere et al 2016

30 ExaSky: Conservative Conservatice Reproducing Reproducing Kernel Kernel SPH (Particle SPH (Particle Hydro) Hydro) Triple-point shock test with CRKSPH, Frontiere et al 2016 Upcoming Frontiere, Raskin, Owen, J. Comp. Phys. (2017); arxiv: [physics.comp-ph] Blob test, Frontiere et al 2016

31 Science Reach/Systematics/ Dependencies What can CMB clusters + LSST clusters do, how much better than S3+LSST? Do we need S4 to reach interesting depth or would more time with existing large aperture facilities (SPT, ACT) be enough? Catalog-based modeling underway! Modeling selection (what is going on in the highest-z clusters? [not foregrounds per se]); false associations; incomplete follow-up (can we get all the telescope time we need to follow up high-z clusters?) Learning a lot from S1-S3 experiments; Telescope access open question! MASS CALIBRATION Optical Weak lensing systematics: shear bias, photo-zs, cluster member contamination, miscentering, profile assumptions Share problems with LSST cluster samples, simulation + data driven efforts underway to tackle these issues! CMB weak lensing biases: tsz, ksz, CIB+Synchrotron from cluster members Correlated Observables - Simulations, targeted followup observations Theoretical Mass Function -> Observed cluster relation (differences in halo catalogs, observer definition of clusters, etc)