Toward Cosmicflows-4: The HI data catalog

Dupuy, Alexandra; Courtois, H. M.; Guinet, D.; Tully, R. Brent; Kourkchi, Ehsan

doi:10.1051/0004-6361/202039025

Cited by 6 publications

(4 citation statements)

References 36 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Nowadays, wide-field optical, infrared, and H I radio surveys provide access to much larger samples. Specifically, here, we make use of serendipitous SDSS DR12 u,g,r,i,z optical imaging (Alam et al 2015), WISE W1 and W2 infrared imaging (Wright et al 2010;Mainzer et al 2011), and Arecibo Legacy Fast ALFA Survey (ALFALFA) neutral hydrogen spectral detections (Haynes et al 2018), supplemented in the radio with pointed observations with the Green Bank Telescope and Parkes Telescope (Dupuy et al 2021).…”

Section: Baryonic Tfrmentioning

confidence: 99%

Cosmicflows-4

Tully

Kourkchi

Courtois

et al. 2023

ApJ

View full text Add to dashboard Cite

With Cosmicflows-4, distances are compiled for 55,877 galaxies gathered into 38,065 groups. Eight methodologies are employed, with the largest numbers coming from the correlations between the photometric and kinematic properties of spiral galaxies (TF) and elliptical galaxies (FP). Supernovae that arise from degenerate progenitors (type Ia SNe) are an important overlapping component. Smaller contributions come from distance estimates from the surface brightness fluctuations of elliptical galaxies and the luminosities and expansion rates of core-collapse supernovae (SNe II). Cepheid period–luminosity relation and tip of the red giant branch observations founded on local stellar parallax measurements along with the geometric maser distance to NGC 4258 provide the absolute scaling of distances. The assembly of galaxies into groups is an important feature of the study in facilitating overlaps between methodologies. Merging between multiple contributions within a methodology and between methodologies is carried out with Bayesian Markov chain Monte Carlo procedures. The final assembly of distances is compatible with a value of the Hubble constant of H 0 = 74.6 km s−1 Mpc−1 with the small statistical error of ±0.8 km s−1 Mpc−1 but a large potential systematic error of ∼3 km s−1 Mpc−1. Peculiar velocities can be inferred from the measured distances. The interpretation of the field of peculiar velocities is complex because of large errors on individual components and invites analyses beyond the scope of this study.

show abstract

Section: Baryonic Tfrmentioning

confidence: 99%

Cosmicflows-4

Tully

Kourkchi

Courtois

et al. 2023

ApJ

View full text Add to dashboard Cite

show abstract

“…It was Email: anastasia.ponomareva@physics.ox.ac.uk first used as a redshift independent tool to measure distances to galaxies, with the aim to measure the peculiar velocities and reconstruct local galaxy flows (e.g. Courtois et al 2012;Tully et al 2013Tully et al , 2014Tully et al , 2019Dupuy et al 2021). Since then, it has been extensively studied in the field of galaxy formation and evolution.…”

Section: Introductionmentioning

confidence: 99%

MIGHTEE-H i: the baryonic Tully–Fisher relation over the last billion years

Ponomareva

Mulaudzi

Maddox

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Using a sample of 67 galaxies from the MIGHTEE Survey Early Science data we study the H i-based baryonic Tully-Fisher relation (bTFr), covering a period of ∼one billion years (0 ≤ z ≤ 0.081). We consider the bTFr based on two different rotational velocity measures: the width of the global H i profile and Vout, measured as the outermost rotational velocity from the resolved H i rotation curves. Both relations exhibit very low intrinsic scatter orthogonal to the best-fit relation (σ⊥ = 0.07 ± 0.01), comparable to the SPARC sample at z ≃ 0. The slopes of the relations are similar and consistent with the z ≃ 0 studies ($3.66^{+0.35}_{-0.29}$ for W50 and $3.47^{+0.37}_{-0.30}$ for Vout). We find no evidence that the bTFr has evolved over the last billion years, and all galaxies in our sample are consistent with the same relation independent of redshift and the rotational velocity measure. Our results set up a reference for all future studies of the H i-based bTFr as a function of redshift that will be conducted with the ongoing deep SKA pathfinders surveys.

show abstract

“…Values for the integrated H flux 𝐹 21 are drawn from two sources. One is the All Digital H file posted in the Extragalactic Distance Database 1 (Courtois et al 2009;Dupuy et al 2021). This compilation for more than 20,000 galaxies draws on observations from the Green Bank 100-meter, 300-foot, and 140-foot telescopes, the Arecibo Telescope, the Parkes Telescope, the Nancay Telescope, and the Effelsberg Telescope.…”

Section: Gas Massmentioning

confidence: 99%

“…The bias arises because the primary selection of targets comes from H surveys that are flux limited, particularly the dominant ALFALFA survey (Haynes et al 2018). See Figure 4 and Dupuy et al (2021) Figure 3. Photometry is comfortably available for any galaxy that meets the H detection criterion.…”

Section: H Flux Biasmentioning

confidence: 99%

Cosmicflows-4: The Baryonic Tully-Fisher Relation Providing ~10,000 Distances

Kourkchi,

Tully,

Courtois

et al. 2022

Preprint

View full text Add to dashboard Cite

The interstellar gas in spiral galaxies can constitute a significant fraction of the baryon mass and it has been demonstrated that the sum of stellar and gas components correlates well with the kinematic signature of the total mass content, the widths of H line profiles. The correlation of baryonic mass with H line widths is used here to obtain distances for 9984 galaxies extending to ∼ 0.05𝑐. The sample is H flux limited and a correction is required to account for an H selection bias. The absolute scale is established by 64 galaxies with known distances from studies of Cepheid variables and/or the magnitudes of stars at the tip of the red giant branch. The calibration of the baryonic relationship results in a determination of the Hubble constant of 𝐻 0 = 75.5 ± 2.5 km s −1 Mpc −1 . The error estimate is statistical. This material will be combined with contributions from other methodologies in a subsequent article where systematic uncertainties will be investigated.

show abstract

Toward Cosmicflows-4: The HI data catalog

Cited by 6 publications

References 36 publications

Cosmicflows-4

Cosmicflows-4

MIGHTEE-H i: the baryonic Tully–Fisher relation over the last billion years

Cosmicflows-4: The Baryonic Tully-Fisher Relation Providing ~10,000 Distances

Contact Info

Product

Resources

About