 2020, ApJ, 902, 145 Cosmicflows 4: The Catalog of ~10000 Tully-Fisher Distances Ehsan Kourkchi, R Brent Tully, Sarah Eftekharzadeh, Jordan Llop, Helene M Courtois, Daniel Guinet, Alexandra Dupuy, James D Neill, Mark Seibert, Michael Andrews, Juana Chuang, Arash Danesh, Randy Gonzalez, Alexandria Holthaus, Amber Mokelke, Devin Schoen, Chase Urasaki We present the distances of 9792 spiral galaxies lying within 15,000 km/s using the relation between luminosity and rotation rate of spiral galaxies. The sample is dominantly, but not exclusively, drawn from galaxies detected in the course of the ALFALFA HI survey with the Arecibo Telescope. Relations between HI line widths and luminosity are calibrated at SDSS u, g, r, i, z bands, and WISE W1 and W2 bands. By exploiting secondary parameters, particularly color indices, we address discrepancies between measured distances at different wavebands with unprecedented detail. We provide a catalog that includes reduced kinematic, photometric, and inclination parameters. A machine learning algorithm is described based on the random forest technique that predicts the dust attenuation in spirals lacking infrared photometry. A value of the Hubble Constant is determined of H0 = 75.1+-0.2 (stat.), with potential systematics up to +-3 km/s/Mpc. Acknowledgments ...
We are pleased to acknowledge the citizen participation to scientific research of undergraduate students at University of Hawaii, members of amateurs astronomy clubs in France Planétarium de Vaulx-en-Velin, Association Clair d’étoiles et Brin d’jardin, Société astronomique de Lyon, Club d’astronomie Lyon Ampère, Club d’astronomie des monts du lyonnais, Club d’astronomie de Dijon, and friends who helped us with measuring inclinations of spiral galaxies in our sample. An application to automatically find the the spatial inclination of Spiral Galaxies using Convolutional Neural Network. The model has been implemented in TensorFlow and uses the outputs of the Galaxy Inclination Zoo for ~10,000 spirals.  For this demo version, the JPG colorful images are taken from the SDSS skyserver. In terms of image quality, SDSS images are nice and homogeneous across the sample. The aligned version of images are used, because finding the semi-major axis of spirals and hence their position angles are fairly easy tasks for other tools.
1,500 randomly chosen images are set aside (we didn't use them in the training process) to check the reliability of the resulting network. In the end, we could generate a model that outputs inclinations with an RMS of 3 degrees. This model is now available to test on any arbitrary spiral galaxy with the SDSS coverage. Please follow this link and open the online application: http://edd.ifa.hawaii.edu/incNET/
We are glad to announce that the first paper of a series of papers to generate the Cosmicflows-4 distance catalog is accepted for publication in the Astrophysical Journal (2019, ApJ, 884, 82). This paper would not have been possible without the output results of the Galaxy Inclination Zoo collaborative tool. The pdf version of this paper is available here: https://arxiv.org/pdf/1909.01572.pdf We are pleased to acknowledge the citizen participation to scientific research of undergraduate students at University of Hawaii, members of amateurs astronomy clubs in France Planétarium de Vaulx-en-Velin, Association Clair d’étoiles et Brin d’jardin, Société astronomique de Lyon, Club d’astronomie Lyon Ampère, Club d’astronomie des monts du lyonnais, Club d’astronomie de Dijon, and friends who helped us with measuring inclinations of spiral galaxies in our sample. The project is still going on and we hope to get more exciting scientific results soon. 
In this presentation, I am talking a little bit about the current status of the project.
The main goal of our research is to map out the density structure of matter in the local universe. To do so, we need to measure the relative velocity of galaxies, known as peculiar velocities. However, as we observe galaxies from the Earth, the measured radial velocity of a galaxy is a superposition of the global Hubble expansion rate and the peculiar velocities. This means that to extract galaxies peculiar velocities, we need to measure their physical distances, and then subtract the resulting Hubble expansion rate from the measured radial velocities. Using the resulting peculiar velocities, later we can recover the underlying density field and discover structures like our home supercluster known as Laniakea.
But the question is that how we measure the distances of galaxies. There are many different methods to measure distances, and each one only works with specific objects. In this research we focus on only Spiral galaxies. There is a well-known relationship between the absolute luminosity of spiral galaxies and how fast they rotate. In Astronomy. this famous relationship is known as Tully-Fisher relationship. Intuitively, one expects that more massive galaxies to be brighter and rotate faster. If we measure how fast a galaxy rotates, then we can estimate its absolute luminosity and compare it with its apparent luminosity that we observe. The difference between absolute and apparent luminosity gives us to the actual distances of galaxies.
With all of that in mind, to achieve our goal we need to measure two different quantities. First, we need to measure the rotation velocity of galaxies, which results in their absolute luminosity if we use the Tully-Fisher relationship that connects rotation rate and luminosity. Second, we need to measure the apparent magnitude of galaxies, which together with the obtained absolute luminosity from the previous step, it gives us distances to galaxies. Spiral galaxies are late-type galaxies with a lot of atomic Hydrogen gas which undergoes star formation. The hydrogen atom consists of one proton and one electron. Each hydrogen atom can be found in two different states. In one state, both electron and proton have the same spin directions, and in the other state, electron and proton have opposite spin directions. The opposite spin direction has slightly lower energy level and the transition from high to low energy states produces radio emission that can be observed at 21 cm. 
Some of this 21 cm emission is blue shifted and some redshifted as the consequence of the rotation of spiral galaxy. This means that the 21 cm emission line is broadened due to rotation. Faster a galaxy rotates, the broader the 21 cm line is. In addition to the rotation, the inclination of the galaxy can change the broadening of the 21 cm emission line. If a galaxy is totally face-on, the observer does not see any rotation and the broadening factor in minimal. As the inclination increases, the 21 cm line-width increases. This means that in addition to the radio observations we need to measure the inclination of galaxies.
The current study mainly focuses on the Northern part of the sky where we had both radio and optical data. This study complements the previous Cosmicflows3 catalog. The absolute luminosity or the mass of spiral galaxies is related to their total rotation velocity. However, what we really get from the HI 21 cm line-widths is the observed rotations that has the projection factor dictated by the galaxy inclination. Therefore, it is important to measure the inclination of galaxies with high accuracy. If a galaxy is face-on, its inclination is 0 and all edge-on galaxies have the inclination of 90 degrees.
So far, all users together have spent more than 1,100 hours on this project. About 5,000 galaxies have been already rejected due to the poor quality of images or bad HI profiles which made them bad candidates for the distance measurements using TF relationship. For those galaxies that have not been rejected, we have made sure that there are at least 3 different measurements done by different users. This increases the accuracy of the final results as we use the median of all measurements. If a user makes a terrible mistake and introduces an outlier which is not consistent with other measurements, that measurement would be later removed. At this time, we have enough information and data to move on to the next level of analysis and prepare the next generation of distance catalog using which we can find more local galaxy structures, like Laniakea. I would like to thank all of those who have already participated or will participate in this project. With more measurements, we can better understand the nature of uncertainties and minimize them, which leads us to better and more accurate distance measurements required for Cosmicflows calculations. All the final products and data catalogs would be available to public through the Extra-Galactic Distance Data-Base. I appreciate all of your comments and suggestions that help us with improving this process. 
We reject all mergers and interacting galaxies with disturbed structures. The following galaxy (pgc21673) is an interesting case where another face-on galaxy is overlapping the original galaxy.
  Red points represent the geographical distribution of all users who are participating in this project. This plot compares my measurements against the median measurements done by the other users.
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Left top panel shows the statistics of the sorted galaxies.The blue bar represents the total number of candidates in our catalog. The red column shows how many galaxies have at least one measurement. The yellow and green bars display the number of galaxies with at least 2 and 3 measurements, respectively.
Left bottom panel shows the number of sorted galaxies as a function of time (this includes all visits: practice, training, calibration, etc). |
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If the HI profile is missing (e.g. the left panel above), treat the galaxy as it has a perfect profile. Although this means that HI profile is not available in our database, we still have the HI line-width and fluxes necessary for our calculations. In the future these profiles would be also imported into the database.
So, in these cases don't put a flag on the "bad HI profile" and no note regarding HI profile is necessary.
Cosmicflow Project
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