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Getting more out of V/Vm than just the mean

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Dilip G Banhatti (School of Physics, Madurai Kamaraj University, India)

Cosmology and Nongalactic Astrophysics · Submitted 19 Mar 2011

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim The function n(z) can be interpreted in terms of redshift distribution obtained by integrating the radio luminosity function {\rho}(P, z) over luminosities P for the survey limiting flux density S0 = 0.5 Jy. Keywords.

how it is stated · asserted 0.82 read the record →

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arXiv ID1103.3752 (version 2)
Pith IDRMTGZM75, Pith's permanent record of this paper and its review
CitationDilip G Banhatti (School of Physics, India), Madurai Kamaraj University. "Getting more out of V/Vm than just the mean." arXiv:1103.3752 (2011). https://pith.science/paper/RMTGZM75
Claim paper

The compiled record

The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Open the compiled record

Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 5,180 input tokens, $0.0002 reported.

What the abstract itself states, as probabilities: claims first 0.05 · states limitation 0.47 · human participants 0.02 · controlled comparison 0.03 · randomized assignment 0.01 · states quantitative result 0.62 · compares with prior results 0.22 · mentions code or data availability 0.03.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; .

Banhatti (2009) set down the procedure to derive cosmological number density n(z) from the differential distribution p(x) of the fractional luminosity volume relative to the maximum volume, x \equiv V/Vm (0 \leq x \leq 1), using a small sample of 76 quasars for illustrative purposes. This procedure is here applied to a bigger sample of 286 quasars selected from Parkes half-Jansky flat-spectrum survey at 2.7 GHz (Drinkwater et al 1997). The values of n(z) are obtained for 8 values of redshift z from 0 to 3.5. The function n(z) can be interpreted in terms of redshift distribution obtained by integrating the radio luminosity function {\rho}(P, z) over luminosities P for the survey limiting flux density S0 = 0.5 Jy. Keywords. V/Vm - luminosity-volume - cosmological number density - redshift distribution - luminosity function - quasars [Note: This somewhat modified version was submitted to MNRaS on 14 July 2016. It was (almost) rejected, except if thoroughly revised.]

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 Banhatti (2009) set down the procedure to derive cosmological number density n(z) from the differential distribution p(x) of the fractional luminosity volume relative to the maximum volume, x \equiv V/Vm (0 \leq x \leq 1), using a small sample of 76 quasars for illustrative purposes. background 0.98 0.04 0.05 asserted 1.00
s1 This procedure is here applied to a bigger sample of 286 quasars selected from Parkes half-Jansky flat-spectrum survey at 2.7 GHz (Drinkwater et al 1997). method 0.57 0.89 0.05 asserted 1.00
s2 The values of n(z) are obtained for 8 values of redshift z from 0 to 3.5. result 0.84 0.90 0.08 asserted 1.00
s3 The function n(z) can be interpreted in terms of redshift distribution obtained by integrating the radio luminosity function {\rho}(P, z) over luminosities P for the survey limiting flux density S0 = 0.5 Jy. Keywords. interpretation 0.99 0.51 0.13 asserted 0.82
s4 V/Vm - luminosity-volume - cosmological number density - redshift distribution - luminosity function - quasars [Note: This somewhat modified version was submitted to MNRaS on 14 July 2016. background 0.68 0.15 0.03 unclear 0.93
s5 It was (almost) rejected, except if thoroughly revised.] background 0.84 0.29 0.02 asserted 0.88

What kind of paper the classifier reports this is: empirical study 0.83 · evidence from analysis of existing data 1.00.

What was examined, and what was not

sources read
  • arXiv listing abstract v2
not examined
  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers
levels run
  • P abstract
not run
  • S sections
  • T body sentences
  • C citations
  • R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper
Original abstract

Banhatti (2009) set down the procedure to derive cosmological number density n(z) from the differential distribution p(x) of the fractional luminosity volume relative to the maximum volume, x \equiv V/Vm (0 \leq x \leq 1), using a small sample of 76 quasars for illustrative purposes. This procedure is here applied to a bigger sample of 286 quasars selected from Parkes half-Jansky flat-spectrum survey at 2.7 GHz (Drinkwater et al 1997). The values of n(z) are obtained for 8 values of redshift z from 0 to 3.5. The function n(z) can be interpreted in terms of redshift distribution obtained by integrating the radio luminosity function {\rho}(P, z) over luminosities P for the survey limiting flux density S0 = 0.5 Jy. Keywords. V/Vm - luminosity-volume - cosmological number density - redshift distribution - luminosity function - quasars [Note: This somewhat modified version was submitted to MNRaS on 14 July 2016. It was (almost) rejected, except if thoroughly revised.]

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