2024/12/19 by C. Hernández–Monteagudo, A. Balaguera-Antolínez, Hernández-Monteagudo, C. +41 · 1 voice · 1 citation
Engineering · Physics and Astronomy · #Astronomical Observations and Instrumentation #Astronomy and Astrophysical Research #Galaxies: Formation, Evolution, Phenomena
paper · doi:10.33232/001c.142149
openalex created_date 2024/12/21 · openalex publication_date 2025/07/14 · openalex updated_date 2026/07/28
The <em>Javalambre Photometric Local Universe Survey</em> (J-PLUS) is a <em> spectro-photometric</em>survey covering about 3,000~deg <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:msup> <mml:mi/> <mml:mn>2</mml:mn> </mml:msup> </mml:math> in its third data release (DR3), and containing about 300,000 galaxies with high quality ( <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mo>></mml:mo> <mml:mn>0.8</mml:mn> </mml:mrow> </mml:math> ) photometric redshifts (hereafter photo- <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mi>z</mml:mi> </mml:math> s). We use this galaxy sample to conduct a tomographic study of the counts and redshift angular fluctuations under Gaussian shells sampling the redshift range <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mi>z</mml:mi> <mml:mo>∈</mml:mo> <mml:mrow> <mml:mo stretchy="true" form="prefix">[</mml:mo> <mml:mn>0.05</mml:mn> <mml:mo>,</mml:mo> <mml:mn>0.25</mml:mn> <mml:mo stretchy="true" form="postfix">]</mml:mo> </mml:mrow> </mml:mrow> </mml:math> . We confront the angular power spectra of these observables measured under shells centered on 11 different redshifts with theoretical expectations derived from a linear Boltzmann code (). Overall we find that J-PLUS DR3 data are well reproduced by our linear, simplistic model. We obtain that counts (or density) angular fluctuations (hereafter ADF) are very sensitive to the linear galaxy bias <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:msub> <mml:mi>b</mml:mi> <mml:mi>g</mml:mi> </mml:msub> <mml:mrow> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mi>z</mml:mi> <mml:mo stretchy="true" form="postfix">)</mml:mo> </mml:mrow> </mml:mrow> </mml:math> , although weakly sensitive to radial peculiar velocities of the galaxy field, while suffering from systematics residuals for <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mi>z</mml:mi> <mml:mo>></mml:mo> <mml:mn>0.15</mml:mn> </mml:mrow> </mml:math> . Angular redshift fluctuations (ARF), instead, show higher sensitivity to radial peculiar velocities and also higher sensitivity to the average uncertainty in photo- <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mi>z</mml:mi> </mml:math> s (), with no obvious impact from systematics. For <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mi>z</mml:mi> <mml:mo><</mml:mo> <mml:mn>0.15</mml:mn> </mml:mrow> </mml:math> both ADF and ARF agree on measuring a monotonically increasing linear bias varying from <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:msub> <mml:mi>b</mml:mi> <mml:mi>g</mml:mi> </mml:msub> <mml:mrow> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mi>z</mml:mi> <mml:mo>=</mml:mo> <mml:mn>0.05</mml:mn> <mml:mo stretchy="true" form="postfix">)</mml:mo> </mml:mrow> <mml:mo>≃</mml:mo> <mml:mn>0.9</mml:mn> <mml:mo>±</mml:mo> <mml:mn>0.06</mml:mn> </mml:mrow> </mml:math> up to <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:msub> <mml:mi>b</mml:mi> <mml:mi>g</mml:mi> </mml:msub> <mml:mrow> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mi>z</mml:mi> <mml:mo>=</mml:mo> <mml:mn>0.15</mml:mn> <mml:mo stretchy="true" form="postfix">)</mml:mo> </mml:mrow> <mml:mo>≃</mml:mo> <mml:mn>1.5</mml:mn> <mml:mo>±</mml:mo> <mml:mn>0.05</mml:mn> </mml:mrow> </mml:math> , while, by first time, providing consistent measurements of that are <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mo>∼</mml:mo> <mml:mn>40</mml:mn> <mml:mspace width="0.222em"/> <mml:mi>%</mml:mi> </mml:mrow> </mml:math> higher than estimates from the photo- <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mi>z</mml:mi> </mml:math> code , (). As expected, this photo- <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mi>z</mml:mi> </mml:math> uncertainty level prevents the detection of radial peculiar velocities in the modest volume sampled by J-PLUS DR3, although prospects for larger galaxy surveys of similar (and higher) photo- <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mi>z</mml:mi> </mml:math> precision are promising.