Tomography-based observational measurements of the halo mass function via the submillimeter magnification bias

Cueli, Marisol; Bonavera, L.; González‐Nuevo, J.; Crespo, Daniel; Casas, Jérôme; Lapi, A.

doi:10.1051/0004-6361/202142949

Cited by 8 publications

(1 citation statement)

References 62 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Therefore, both samples are not cross-contaminated by each other. For these reasons, SMGs have already been successfully used in magnification bias analyses to investigate the projected mass density profile and concentration of foreground samples of quasi-stellar objects (QSOs; Bonavera et al 2019), for cosmological studies (Bonavera et al 2020;González-Nuevo et al 2021;Bonavera et al 2021b), and to observationally constrain the halo mass function (Cueli et al 2021(Cueli et al , 2022.…”

Section: Introductionmentioning

confidence: 99%

Quasi-stellar objects and galaxy mass density profiles derived using the submillimetre galaxies magnification bias

Crespo

González‐Nuevo

Bonavera

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

Context. The magnification bias on the submillimetre galaxies (SMGs) is a gravitational lensing effect, where the SMGs are used as background lensed galaxies. This effect can be used to investigate the mass density profiles of different types of foreground lenses. Aims. In this work, we want to exploit the magnification bias of the SMGs using two different foreground samples, quasi-stellar objects (QSOs) and galaxies. Our aim is to study and compare their mass density profiles and estimate their masses and concentrations. Methods. The background SMG sample consists of objects observed by Herschel with 1.2 < z < 4.0 (mean redshift at ∼ 2.2). The foreground samples are QSOs with spectroscopic redshifts 0.2 < z < 1.0 (mean redshift at ∼ 0.7) and massive galaxies with also spectroscopic redshifts 0.2 < z< 1.0 (mean redshift at ∼ 0.3). The cross-correlation measurements are estimated with the Davis-Peebles estimator by stacking the SMG-QSO and SMG-galaxy pairs for the two analysed cases, respectively. The advantage of such an approach is that it allows us to study the mass density profile over a wide range of angular scales, from ∼ 2 to ∼ 250 arcsec, including the inner part of the dark-matter halo (≲ 100 kpc). Moreover, the analysis is carried out by combining two of the most common theoretical mass density profiles in order to fit the cross-correlation measurements.Results. The measurements are correctly fitted after splitting the available angular scales into an inner and an outer part using two independent mass density profiles, one for each region. In particular, for the QSOs, we obtain masses of log 10 (M/M ⊙ ) = 13.51 ± 0.04 and of log 10 (M/M ⊙ ) =13.44±0.17 for the inner and outer parts, respectively. The estimated masses for the galaxy sample are log 10 (M/M ⊙ ) = 13.32 ± 0.08 and log 10 (M/M ⊙ ) =12.78±0.21 for the inner and outer parts, respectively. The concentrations for the inner part are much higher than those for the outer region for both samples: C = 6.85 ± 0.34 (inner) and C =0.36±0.18 (outer) for the QSOs and C = 8.23 ± 0.77 (inner) and C =1.21±1.01 (outer) for the galaxies. Conclusions. In both samples, the inner part has an excess in the mass density profile with respect to the outer part for both QSOs and galaxy samples. We obtain similar values for the central mass with both samples, and they are also in agreement with those of galaxy clusters results. However, the estimated masses for the outer region and the concentrations of the inner region both vary with lens sample. We believe this to be related to the probability of galactic interactions and/or the different evolutionary stages.

show abstract

Section: Introductionmentioning

confidence: 99%

Quasi-stellar objects and galaxy mass density profiles derived using the submillimetre galaxies magnification bias

Crespo

González‐Nuevo

Bonavera

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

Methodological refinement of the submillimeter galaxy magnification bias

Bonavera,

Cueli,

González-Nuevo

et al. 2024

A&A

View full text Add to dashboard Cite

Context. This work focuses on the submillimeter galaxy magnification bias, specifically in the tomographic scenario. It builds upon previous works, while utilising updated data to refine the methodology employed in constraining the free parameters of the halo occupation distribution model and cosmological parameters within a flat ΛCDM model. Aims. This work aims to optimise CPU time and explore strategies for analysing different redshift bins, while maintaining measurement precision. Additionally, it seeks to examine the impact of excluding the GAMA15 field, one of the H-ATLAS fields that was found to have an anomalous strong cross-correlation signal, and increasing the number of redshift bins on the results. Methods. The study uses a tomographic approach, dividing the redshift range into a different number of bins and analysing cross-correlation measurements between H-ATLAS submillimeter galaxies with photometric redshifts in the range 1.2 < z < 4.0 and foreground GAMA galaxies with spectroscopic redshifts in the range 0.01 < z < 0.9. Interpreting the weak lensing signal within the halo model formalism and carrying out a Markov chain Monte Carlo algorithm, we obtain the posterior distribution of both halo occupation distribution and cosmological parameters within a flat ΛCDM model. Comparative analyses are conducted between different scenarios, including different combinations of redshift bins and the inclusion or exclusion of the GAMA15 field. Results. The mean-redshift approximation employed in the “base case” yields results that are in good agreement with the more computationally intensive “full model” case. Marginalised posterior distributions confirm a systematic increase in the minimum mass of the lenses with increasing redshift. The inferred cosmological parameters show narrower posterior distributions compared to previous studies on the same topic, indicating reduced measurement uncertainties. Excluding the GAMA15 field demonstrates a reduction in the cross-correlation signal, particularly in two of the redshift bins, suggesting a sample variance within the large-scale structure along the line of sight. Moreover, extending the redshift range improves the robustness against the sample variance issue and produces similar, but tighter constraints compared to excluding the GAMA15 field. Conclusions. The study emphasises the importance of considering sample variance and redshift binning in tomographic analyses. Increasing the number of independent fields and the number of redshift bins can minimise both the spatial and redshift sample variance, resulting in more robust measurements. The adoption of additional wide area field observed by Herschel and of updated foreground catalogues, such as the Dark Energy Survey or the future Euclid mission, is important for implementing these approaches effectively.

show abstract

Mass density profiles at kiloparsec scales using the sub-millimetre galaxies magnification bias

Crespo,

González-Nuevo,

Bonavera

et al. 2024

A&A

View full text Add to dashboard Cite

Gravitational lensing is a powerful tool for studying the distribution of mass in the Universe. Understanding the magnification bias effect in gravitational lensing and its impact on the flux of sub-millimetre galaxies (SMGs) is crucial for accurate interpretations of observational data. This study aims to investigate the magnification bias effect in the context of gravitational lensing and analyse the mass density profiles of different types of foreground lenses, including quasi-stellar objects (QSOs), galaxies, and galaxy clusters. The specific goals are to compare the lens types, assess the impact of angular resolution on the analysis, and determine the adequacy of theoretical mass density profiles in explaining the observed data. The magnification bias was estimated using the cross-correlation function between the positions of background SMGs and foreground lens samples. Stacking techniques were employed to enhance the signal at smaller angular separations, and the more precise positions from the WISE catalogue were utilised to improve positional accuracy. Four different theoretical mass density profiles were analysed to extract additional information. The cross-correlation measurements revealed distinctive central excess and outer power-law profiles, with a lack of signal in the intermediate region. The lens types exhibited varying signal strengths, with QSOs producing the strongest signal and galaxy clusters showing weaker signals. The analysis of mass density profiles indicated limitations in the selected profiles' ability to explain the observed data, highlighting the need for additional considerations. The lack of extended emission in the QSO sample suggested possible influences from close satellites along the line of sight in the other lens types. The study provides valuable insights into the magnification bias effect and mass density profiles in gravitational lensing. The results suggest the presence of isolated galactic halos and the importance of considering environmental factors and close satellites in future investigations. The derived masses and best-fit parameters contribute to our understanding of lensing systems and provide constraints on the nature of central galaxies. Notably, the intriguing lack of signal around 10 arcsec challenges current understanding and calls for further quantitative analysis and confirmation of the observed feature.

show abstract

Tomography-based observational measurements of the halo mass function via the submillimeter magnification bias

Cited by 8 publications

References 62 publications

Quasi-stellar objects and galaxy mass density profiles derived using the submillimetre galaxies magnification bias

Quasi-stellar objects and galaxy mass density profiles derived using the submillimetre galaxies magnification bias

Methodological refinement of the submillimeter galaxy magnification bias

Mass density profiles at kiloparsec scales using the sub-millimetre galaxies magnification bias

Contact Info

Product

Resources

About