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The Arecibo Pisces-Perseus Supercluster Survey (APPSS) is an observing project by the Undergraduate ALFALFA Team, aimed at determining the mass of the Pisces Perseus Supercluster through measurement of peculiar velocities from HI line detections. The survey targeted approximately 600 galaxies selected based on SDSS and GALEX photometry as likely to contain HI. We reduced Arecibo L-Band Wide observations for 90 galaxies near declination 25 degrees, 40 of which showed HI emission. 58% of those 40 galaxies were below 10,000 km/s recession velocity and thus will provide useful information to draw conclusions from. We determined the recession velocity, velocity width, and HI line flux for each detection. We discuss our results for APPSS galaxies and for ALFALFA detections near this declination strip. By combining results from all strips, APPSS will determine which galaxies are associated with the Pisces-Perseus Supercluster, and their peculiar velocities will be measured via the baryonic Tully-Fisher relation. This work has been supported by NSF grants AST-1211005 and AST-1637339. 

The Arecibo Pisces-Perseus Supercluster Survey (APPSS) will provide strong observational constraints on the mass-infall rate onto the main filament of the Pisces-Perseus Supercluster. The survey data consist of HI emission-line spectra of cluster galaxy candidates, obtained primarily at the Arecibo Observatory (with ALFA as part of the ALFALFA Survey and with the L-Band Wide receiver as part of APPSS observations). Here we present the details of the data reduction process and spectral-analysis techniques used to determine if a galaxy candidate is at a velocity consistent with the Supercluster, as well as the detected HI-flux and rotational velocity of the galaxy, which will be used to estimate the corresponding HI-mass. We discuss the results of a preliminary analysis on a subset of the APPSS sample, corresponding to 98 galaxies located within ~1.5° of DEC = +35.0°, with 65 possible detections. We also highlight several interesting emission-line features and galaxies discovered during the reduction and analysis process and layout the future of the APPSS project. This work has been supported by NSF grants AST-1211005 and AST-1637339. 

The Arecibo Pisces-Perseus Supercluster Survey (APPSS) aims to exploit the Baryonic Tully-Fisher Relation to derive distances and peculiar velocities of galaxies in and near the main ridge of the Pisces-Perseus Supercluster (PPS), one of the most prominent features of the Cosmic Web in the nearby Universe. The sample of galaxies contains ~ 600 sources in the low-mass range (8 < log MHI / M⊙ < 9). The source selection was based on the ALFALFA HI survey, SDSS and GALEX photometric data. The sample galaxies have HI masses just below the ALFALFA detection threshold, and were selected to be blue disk systems (low surface brightness sources from optical photometry data). The HI data were obtained at the Arecibo Observatory between the years 2015 and 2016. With this sample, the nature of the galaxy population in and around the PPS will be investigated. The HIMF to log MHI ~ 8.0 along the PPS filament will be measured and using the Tully-Fisher relation it will be possible to make a robust measurement of the infall and backflow onto the filamentary structure.APPSS is collaborative project between more than 10 Undergraduate ALFALFA Team institutions in which each group contributes to the analysis of a subset of the HI PPS data. In this poster, we will present the contributions of the U.P.R. team to the APPSS project. We will show the procedure used for the Arecibo HI data analysis, including some examples, and will show our preliminary results. 

We present results from an ALFALFA HI study to examine whether the cold gas reservoirs of galaxies are inhibited or enhanced in large-scale filaments, and we discuss implications for follow-up work using the new Arecibo Pisces-Perseus Supercluster survey (APPSS). From the ALFALFA survey, we find that the HI deficiency for galaxies in the range 10^8.5-10^10.5 solar masses decreases with distance from the filament spine, suggesting that galaxies are cut off from cold gas, possibly by heating or by dynamical detachment from the smaller-scale cosmic web. This contrasts with previous results for larger galaxies in the HI Parkes All-Sky Survey. We discuss the prospects for elucidating this apparent dependence on galaxy mass with data from the APPSS, which will extend to smaller masses. We also find that the most gas-rich galaxies at fixed local density and stellar mass are those in small, correlated ``tendril” structures within voids: although galaxies in tendrils are in significantly denser environments, on average, than galaxies in voids, they are not redder or more HI deficient. This work has been supported by NSF grants AST-1211005 and AST-1637339.