研究目的
To measure the cross-correlation between cosmic far-infrared background anisotropies and large-scale structures (specifically luminous red galaxies) to constrain the halo mass hosting star-forming galaxies, the bias, and dust temperature, and to discuss implications for the star formation history and galaxy-dark matter link.
研究成果
The cross-correlation measurements confirm a most efficient halo mass for star-forming galaxies of log(Meff/M☉) = 12.84 ± 0.15, a bias bFIRB ~ 1.45, and a mean dust temperature Td = 26 K at z ~ 0.55. These results align with previous studies and highlight the potential of cross-correlations with FIRB anisotropies to probe the star formation history and the connection between galaxies and dark matter, with future studies needed to explore redshift evolution and reduce systematic uncertainties.
研究不足
The analysis is limited to a narrow redshift bin (z ~ 0.55), which restricts the ability to study redshift evolution of parameters. The SED parameters (β and γ) are fixed due to insufficient data constraints. Potential systematics from Galactic dust and instrument noise affect the measurements, and cross-correlations with other tracers like quasars were not included due to unresolved systematics.
1：Experimental Design and Method Selection:
The study uses cross-correlation analysis in harmonic space with the pseudo-C? technique to measure cross-power spectra between FIRB maps and LRG density maps. An extended halo model is employed to connect galaxy luminosity to host halo mass, assuming a log-normal function for the luminosity-mass relation and a modified black body SED for galaxies.
2：Sample Selection and Data Sources:
LRGs are selected from SDSS-III DR8 catalog with photometric redshifts 0.45 < z < 0.65, covering 7760 deg2 in the northern hemisphere. FIRB data come from Planck (353, 545, 857 GHz) and IRIS (3000 GHz) maps.
3：45 < z < 65, covering 7760 deg2 in the northern hemisphere. FIRB data come from Planck (353, 545, 857 GHz) and IRIS (3000 GHz) maps.
List of Experimental Equipment and Materials:
3. List of Experimental Equipment and Materials: Instruments include the Planck satellite, IRAS satellite (IRIS reprocessing), and SDSS telescope. Software includes HEALPix for map pixelization and analysis, CAMB for power spectrum computations, and CosmoMC for Markov chain analysis.
4：Experimental Procedures and Operational Workflow:
Maps are created using HEALPix pixelization. Cross-power spectra are computed using anafast from HEALPix, with masking for Galactic emission and point sources. Error bars are estimated via Monte Carlo simulations with 500 realizations. Null tests (random maps and rotation tests) are performed to check for systematics.
5：Data Analysis Methods:
Data are analyzed using the Limber approximation for power spectra. Parameters (Meff, Td, L0) are constrained via Markov chain Monte Carlo with priors. Power-law fits are also applied for comparison.
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