Dark Energy Survey: early SV and Y1 large-scale structure results

Talk given at the APS meeting about early DES results (galaxy clustering, etc), touching arXiv:1507.05647 and other papers of the SV batch, as well as preliminary Y1 results

Transcript

1. Boris Leistedt @ixkael, New York University On behalf of the DES LSS Working Group PROBING THE LARGE SCALE STRUCTURE OF THE UNIVERSE WITH THE DARK ENERGY SURVEY (DES)
2. dark energy™ microscopic origin cosmological constant problem 70% 24% 5% 1% dark matter™ microscopic origin detailed cosmological impact baryons galaxy formation gastrophysics the rest neutrinos, radiation, anti-matter, etc
3. experimental landscape
4. Unlensed Lensed With Shape Noise Without Shape Noise galaxy distribution = indirect probe of dark matter cosmic shear = more direct probe of dark matter
5. spectroscopic vs photometric surveys
6. spectroscopic SEDs types redshifts shallow no shear
7. CCD images deep shear no types no redshifts photometric
8. spectroscopic photometric types + redshifts shallow no types / redshifts deep credit: Aragon-Calvo et al (2014) z z 3D 3D + 2+1D
9. The Dark Energy Survey
10. 3 deg2 FOV, 570 Mpixel camera on Blanco telescope (4m, CTIO) 2013-2018, 300 collaborators ~300 international collaborators The Dark Energy Survey
11. Over 60 papers already! Some highlights: ‣ Galaxy-Galaxy Lensing, Clampitt et al, arXiv:1603.05790 ‣ Cosmology constraints from shear peak statistics, Kacprzak et al, arXiv:1603.05040 ‣ Detection of the kinematic Sunyaev-Zel'dovich effect (DES Y1), Soergel et al, arXiv:1603.03904 ‣ DECam Search for an Optical Counterpart to the First Advanced LIGO Gravitational Wave Event GW150914, Soares-Santos et al, arXiv:1602.04198 ‣ Cosmic Shear Measurements, Becker et al, arXiv:1507.05598 ‣ Cosmology from Cosmic Shear, arXiv:1507.05552 ‣ CMB lensing tomography, T. Giannantonio et al, arXiv:1507.05551 ‣ Wide-Field Lensing Mass Maps, Chang et al, arXiv:1505.01871
14. reduction of single-epoch images coaddition into deep images object detection flux + shape measurements } is hard
15. Science Goals ‣ Test the standard model / search for new physics: dark matter, dark energy, modified gravity, expansion history, extreme objects, etc ‣ 4 standard observational probes: galaxy clustering, galaxy lensing, supernovae, clusters ‣ Extras: cross-correlations with CMB & other galaxy surveys, quasars, extreme objects, voids, etc HUGE data set & high quality: lots of legacy data + science
16. Results from DES SV & Y1 data
17. Full survey: 5000 deg2 grizY to 24th mag Science Verification: ~150 deg2 to full depth Year 1: ~1500 deg2 but shallower In the can (Y2-3): 5000 deg2 deeper than Y1
18. DES Science Verification (SV) data ‣ Early data, excellent quality ‣ Benchmark galaxy sample: ~120 deg2, imag < 22.5, cuts similar to CFHTLenS 55 50 45 90 85 80 75 70 65 60 4 5 6 7 8 9 ng [arcmin 2] 0.2 0.4 0.6 0.8 1.0 1.2 1.4 0 1 2 3 4 z 10-6 ¥ dnêdz HzL TPZ 0.2 < zphot < 0.4 0.4 < zphot < 0.6 0.6 < zphot < 0.8 0.8 < zphot < 1.0 1.0 < zphot < 1.2 0.2 0.4 0.6 0.8 1.0 1.2 1.4 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 z 10-6 ¥ dnêdz HzL BPZ 0.2 < zphot < 0.4 0.4 < zphot < 0.6 0.6 < zphot < 0.8 0.8 < zphot < 1.0 1.0 < zphot < 1.2
19. Angular clustering measurements Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ 0.01 0.1 1 0.0 0.1 0.2 0.3 q @degD wHqL Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê 0.01 0.05 0.1 1.0 < zphot < 1.2 Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê 0.1 1 0.00 0.02 0.04 0.06 0.08 q @degD wHqL Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê 0.01 0.1 0.1 0.5 0.8 < zphot < 1.0 Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê 0.1 1 0.00 0.02 0.04 0.06 0.08 0.10 q @degD wHqL Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê 0.01 0.1 0.01 0.1 0.6 < zphot < 0.8 Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ 0.1 1 0.00 0.02 0.04 0.06 0.08 q @degD wHqL Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê 0.01 0.1 0.01 0.1 0.4 < zphot < 0.6 Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ ‡ 0.1 1 0.00 0.01 0.02 0.03 0.04 0.05 0.06 q @degD wHqL Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê Ê 0.01 0.1 0.01 0.1 0.2 < zphot < 0.4 Crocce et al (MNRAS 2015, arXiv:1507.05360) With corrections for spatial systematics
20. Observing conditions & systematics Leistedt et al (ApJS 2015, arXiv:1507.05647) Mapping & projecting image properties Useful for null tests, systematics checks, …
21. Robustness against systematics Crocce et al, Leistedt et al (arXiv:1507.05360, 1507.05647)
22. Cross-correlation with CMB lensing Giannantonio et al (MNRAS 2015, arXiv:1507.05551) X
23. Galaxy bias measurements Chang et al (2015, arXiv:1601.00405), Crocce et al (2015, arXiv:1507.05360), Giannantonio et al (2015, arXiv:1507.05551), Pujol et al (2015, arXiv:1601.00160) Ratio between DES galaxies and lensing mass maps (Chang+) DES galaxy clustering measurements (Crocce+) DES galaxies / CMB lensing cross-corrrelations (Giannantonio+)
24. BALROG 10 3 10 2 10 1 100 101 ✓ [deg] 10 4 10 3 10 2 10 1 100 w(✓) DES B alrog DES Uniform COSMOS 60 55 50 45 6:00h 5:40h 5:20h 5:00h 4:40h 4:20h 4:00h DES 60 55 50 45 Suchyta et al (MNRAS 2015, arXiv:1507.08336) 60 55 50 45 6:00h 5:40h 5:20h 5:00h 4:40h 4:20h 4:00h DES 60 55 50 45 6:00h 5:40h 5:20h 5:00h 4:40h 4:20h 4:00h B alrog 10 15 20 25 30 ng [arcmin 2] Inject simulated galaxies in real DES images => excellent tracers of depth + systematics => deeper clustering measurements
25. Clustering of Y1 Red Galaxies ‣ Red galaxies: high bias, good photo-z’s ‣ Optimized for 0.6 < z < 1 BAO measurements ‣ Good 3D clustering results, 5% BAO precision expected D ES Prelim inary
26. Kinematic Sunyaev Zel’dovich effect (DES:Y1xSPT) ‣ Pairwise estimator, usually using spectroscopic surveys ‣ 5,500 clusters from DES Y1 ‣ 4.2σ detection ‣ Exceptional probe of gravity and cluster physics! Soergel et al (2016, arXiv:1603.03904) 0 50 100 150 200 250 300 comoving pair separation [Mpc] 12 10 8 6 4 2 0 2 4 pairwise kSZ amplitude [µK] fit : ¯ te = (3.75±0.89)·10 3 DES⇥SPT 300.0° 330.0° 0.0° 30.0° 60.0° 90.0° RA -70.0° -60.0° -50.0° -40.0° Dec -0.5 0.0 0.5 1.0 1.5 Relative Cluster Density
27. conclusions
28. SV data yielded excellent results, including: • galaxy clustering + lensing measurements • cross-correlations with external data + new probes Y1 data analyzes being finalized, expected to give: • precise BAO measurements • cosmology results using combined probes Y2-Y3 data in the can DES = high quality, rich data allowing precise multi- probe cosmological tests + lots of new science