Dusty Starforming Galaxies: Astrophysical and Cosmological Relevance

Transcription

1 Dusty Starforming Galaxies: Astrophysical and Cosmological Relevance Andrea Lapi SISSA, Trieste, Italy INFN-TS, Italy INAF-OATS, Italy in collaboration with F. Bianchini, C. Mancuso C. Baccigalupi, L. Danese

2 A new window on the Universe has been disclosed

3 and has unveiled a new galaxy population: DSFGs Mancuso+16b

4 DSFGs are heavily dust obscured, missed in the UV Mancuso+16a Tadaki+16

5 DSFGs are main contributors to cosmic star formation at z>1 Lapi+17

6 Aside: cosmic reionization and constraints on DM particle mass Lapi+15,17

7 DSFGs are the progenitors of massive ellipticals (cf. JWST) Mancuso+16a

8 Many DSFGs are young, gas rich outliers in GMS (cf. ALMA) Mancuso+16b

9 DSFGs are parent hosts of supermassive BHs GW (cf. elisa) Aversa+15

10 In DSFG coevolution of SF and BH accretion caught in the act Mancuso+16b

11 DSFGs as targets for ultradeep radio surveys (cf. SKA) Mancuso+17, in prep

12 DSFGs can be strongly gravitationally lensed Negrello+10

13 in an appreciable number of instances (cf. SPT, balloons) Mancuso+16a Negrello+14,17

14 In the next future lenses can be exploited for cosmology Eales+16

15 or to study astrophysics around the central BH (ALMA) Dye+16

16 A new paradigm of in-situ co-evolution is emerging (cf. ALMA) Shi+17 in prep.

17 Xcorr of DSFGs with CMB lensing [I] Meeting ASI-COSMOS Planck coll. 16

18 Xcorr of DSFGs with CMB lensing [II] Meeting ASI-COSMOS Hosts galaxies Light is a (biased) tracer of matter MATTER DISTRIBUTION Lens CMB photons Lensing is insensitive to matter s nature Galaxy fluctuations Matter fluctuations Bias Bianchini+15

19 Xcorr of DSFGs with CMB lensing [III] Bianchini+15

20 Xcorr of DSFGs with CMB lensing [IV] Bianchini+16

21 Summary Points of relevance for COSMOS cosmic reionization & constraints on DM microphysics (e.g. WDM vs. CDM) JWST + CMB exp. Astrophysics of high-redshift galaxies and AGNs control of systematics in future CMB exp. BH merging (GW+astro of accretion) interface with elisa Strong gravitational galaxy-galaxy lensing (DM & DE) wide area, low sensitivity (>10 mjy) mm exp. (balloons?) Xcorrelation studies (DM & DE + GF) interface between CMB pol. exp. with EUCLID and LSS surveys (e.g., delensing) Bottom line strong interlink between Astro & Cosmo

22 Bonus slide

23 XC formalism We introduce an amplitude parameter A and combine Cross- and Auto-spectra to break the degeneracy w/ bias Federico Bianchini 23

24 Herschel-ATLAS Galaxies Optimal tracers: they pierce the distant Universe where the CMB lensing kernel peaks Spec-z Optical photo-z FIR photo-z Pearson+13 Low-z: normal starforming late-type galaxies (Dunne+11; Guo+11) Create two samples with: High-z: dustenshrouded starforming galaxies (Maddox+10;Xia+12) Federico Bianchini 24

25 Galaxies photo-z SED Template Fitting (SMM) Theoretical predictions Create maps Federico Bianchini 25 Budavari+03; Lapi+11; Gonzalez-Nuevo+12; Pearson+13; FB+15

26 Errors & null tests We use our set of 500 CMB lensing and galaxy realizations (w/ statistical properties that match the data) as well as the 100 CMB lensing simulated maps released by Planck team to: evaluate covariances and check the stability of estimated errors verify our pipeline and the reconstructed spectra against the possibility of residual systematic errors by performing null tests Federico Bianchini Mean spectra are consistent w/ null 26

27 2013 vs 2015 DATA Cross spectrum Use MASTER method (pseudo-c l ) to deconvolve for masking and pixel window function 7 bin linearly spaced from Extracted spectra are robust against changes w.r.t. Lensing maps, Catalogs and Masks Federico Bianchini 27

28 DATA spectra Use MASTER method (pseudo-c l ) to deconvolve for masking and pixel window function Null hypothesis rejection (i.e. no correlation between fields) from 10s to 22s Low-l auto-spectrum lack of power Federico Bianchini 28

29 Constraints from joint-analysis Study Bias and Growth (Giannantonio+15; Pullen+15) Gaussian Likelihood + MCMC emcee code (Foreman-Mackey+13)? > Fixed cosmology + bias-dependent covariance A > 2-3 s Federico Bianchini 29

30 Photo-z tests To test the robustness of results against changes in photo-z, we redo the analysis using catalogs adopting the SED of Pearson+13 Cross-spectra are more stable than auto-spectra Auto-spectrum low-z bin anomaly mitigated A = 1 for high-z bin, however bias looks unrealistic Federico Bianchini 30

31 Other tests The correlation of galaxy positions in the two redshift bins: most of the observed signal is consistent with the intrinsic clustering signal of objects Flux threshold at 350 mm: 3 5s Higher S/N sources, smaller number Higher inferred bias for baseline and low-z bin (Malmquist bias) C l gg low-z bin anomaly disappears Federico Bianchini 31

32 CMB Lensing Lensing re-maps the T field Adapted from S. Das slides Lensing Potential Geometry Growth of structures Typical deflections of Smearing of acoustic peaks Generation of non-gaussian features Conversion of E-modes B-modes Contribution from CMB redshift is (well) known Only source for high-z objects Mainly sourced by linear scales (well understood) Federico Bianchini 32

33 Magnification Bias (MB) Lensing of background galaxies by foreground LSS induces and apparent clustering in the sky Modifies observed area changes the objects density (De)magnify observed fluxes Does not depend on tracer bias Gonzalez-Nuevo+14 has shown that the MB is substantial for high-z H-ATLAS selected with same criteria as here Federico Bianchini 33

34 Photo-z Stacked photo-z posterior (work in progress with Andrew Jaffe) Federico Bianchini 34

35 CMB convergence Correlation by eye Sub-mm galaxies trace the peaks of matter density field and are denser in regions where the CMB convergence is enhanced Galaxy density Federico Bianchini 35