We present spectroscopic and photometric data for 920 galaxies selected in 68 fields of the Aquarius Cluster Catalog. Typically, the 15 brightest candidate members with magnitudes in the range 16<b_J_<21 were selected for observations, and ~71% turn out to be cluster members. Using the new redshift determinations, we assign galaxies to groups and clusters, and by including data from the literature we calculate systemic velocities and velocity dispersions for 74 clusters, each with redshifts measured for at least six individual galaxies.
For the first time, we have detected Cepheid variables in the Sculptor Group spiral galaxy NGC 7793. From wide-field images obtained in the optical V and I bands on 56 nights in 2003-2005, we have discovered 17 long-period (24-62 days) Cepheids whose periods and mean magnitudes define tight period-luminosity relations. We use the (V-I) Wesenheit index to determine a reddening-free true distance modulus to NGC 7793 of 27.68+/-0.05mag (internal error) +/-0.08mag (systematic error).
We have detected, for the first time, Cepheid variables in the Sculptor Group SB(s)m galaxy NGC 55. From wide-field images obtained in the optical V and I bands during 77 nights in 2002-2003, we have found 143 Cepheids with periods ranging from 5.6 to 175.9 days; 133 of these objects have periods longer than 10 days, making NGC 55 to date the galaxy with the largest known number of long-period Cepheids in the Sculptor Group.
We have conducted an extensive wide-field imaging survey for Cepheid variables in the Local Group irregular galaxy WLM. From data obtained on 101 nights, we have discovered 60 Cepheids, which include 14 of the 15 Cepheid variables previously detected by Sandage and Carlson. Our Cepheid survey in WLM should be practically complete down to a period of 3-days. Importantly, we have found for the first time a long-period Cepheid (P=54.2-days) in this galaxy, alleviating the problem that WLM with its many blue, massive stars does not contain Cepheids with periods longer than about 10-days.
We have obtained multiobject spectroscopy of luminous blue supergiants in NGC 3109, a galaxy at the periphery of the Local Group at ~1.3Mpc. We present a detailed catalog including finding charts, V and I magnitudes, spectral classifications, and stellar radial velocities. The radial velocities are seen to trace the rotation curves obtained from studies of the H I gas. From quantitative analysis of eight B-type supergiants we find a mean oxygen abundance of 12+log(O/H)=7.76+/-0.07 (1{sigma} systematic uncertainty), with a median result of 7.8. Given its distance, we highlight NGC 3109 as the ideal example of a low-metallicity, dark-matter-dominated dwarf galaxy for observations with the next generation of ground-based extremely large telescopes.
Archive of Nearby Galaxies: Reduce, Reuse, Recycle (ANGRRR)
Short Name:
HST.ANGRRR
Date:
22 Jul 2020 22:28:43
Publisher:
Space Telescope Science Institute Archive
Description:
An archive of stellar photometry for galaxies within 3.5 Mpc, excluding Local Group galaxies, based on primary and parallel wide-filter UV and optical observations taken with HST ACS/WFC or WFPC2.The sample includes all observations taken through Dec. 2008, as well as observations
taken as part of Cycle 16 Supplemental GO programs 11986 and 11987. This release includes the ANGST targets within 3.5 Mpc; these observations
have been rereduced using updated CTE corrections and zeropoints. Galaxies with 3.5 < D <= 5 Mpc will be included in a later release.
We present accurate B1950 and J2000 positions for all confirmed galaxies in the Uppsala General Catalog (UGC, Cat. <VII/26>). The positions were measured visually from Digitized Sky Survey images with rms uncertainties {sigma}<=[(1.2")^2^+({theta}/100)^2^]^1/2^, where is the major-axis diameter. We compared each galaxy measured with the original UGC description to ensure high reliability. The full position list is available in the electronic version only. the major-axis diameter. We compared each galaxy measured with the original UGC description to ensure high reliability. The full position list is available in the electronic version only.
The Arecibo Dual-Beam Survey is a "blind" 21 cm search for galaxies covering ~430deg^2^ of sky. We present the data from the detection survey as well as from the follow-up observations to confirm detections and improve positions and flux measurements. We find 265 galaxies, many of which are extremely low surface brightness. Some of these previously uncatalogued galaxies lie within the zone of avoidance, where they are obscured by the gas and dust in our Galaxy. Eighty-one of these sources are not previously catalogued optically, and there are 11 galaxies that have no associated optical counterpart or are only tentatively associated with faint wisps of nebulosity on the Digitized Sky Survey images. We discuss the properties of the survey, and in particular we make direct determinations of the completeness and reliability of the sample. The behavior of the completeness and its dependencies is essential for determining the H I mass function. We leave the discussion of the mass function for a later paper, but do note that we find many low surface brightness galaxies and seven sources with M_HI_<10^8^M_{sun}_.
The Arecibo Legacy Fast ALFA extragalactic HI survey uses the Arecibo multibeam receiver to survey 7000 square degrees of high galactic latitude sky. Utilizing the high sensitivity of Arecibo, the survey will detect over 20000 HI sources in the local universe. The survey products include catalogs with extracted measurements and HI parameters, as well as integrated HI spectral profiles. The survey is currently served by NED.