- ID:
- ivo://CDS.VizieR/J/AJ/131/2089
- Title:
- Planetary nebulae in NGC 3379 and NGC 3384
- Short Name:
- J/AJ/131/2089
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report on observations of four early-type galaxies performed with the Rutgers Fabry-Perot in order to search for planetary nebulae (PNe) in these systems. The aim is to use the PNe as kinematic tracers of the galaxy potential. We describe our data reduction and analysis procedure and show that the proper calibration of our detection statistic is crucial in getting down to our limiting magnitude of m_5007_=26.1. In the case of the two Leo galaxies, we find moderately sized samples: 54 PNe in NGC 3379 and 50 PNe in NGC 3384; NGC 4636 (two PNe) and NGC 1549 (six PNe) are included for completeness. We present our samples in tabular form, as well as the spectrum for each PN.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/MNRAS/393/329
- Title:
- Planetary nebulae of NGC 4494
- Short Name:
- J/MNRAS/393/329
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present new Planetary Nebula Spectrograph observations of the ordinary elliptical galaxy NGC 4494, resulting in positions and velocities of 255 planetary nebulae out to seven effective radii (25kpc). We also present new wide-field surface photometry from MMT/Megacam, and long-slit stellar kinematics from VLT/FORS2.
- ID:
- ivo://CDS.VizieR/J/ApJ/414/463
- Title:
- Planetary nebula system of NGC 5128
- Short Name:
- J/ApJ/414/463
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the result of a planetary nebula (PN) survey of the nearby giant elliptical galaxy NGC 5128 performed with CCD cameras at the prime focus of the CTIO 4m in telescope. By comparing CCD images centered on the characteristic emission line [O III] {lambda}5007{AA} and on the adjacent continuum, we identify a total of 785 PNs in areas extending 20kpc along the photometric major axis and covering the whole galaxy to 10kpc. From these data, we form a complete sample of 224 PN's extending to a dereddened limiting magnitude of m_5007_=24.8, which extends 1.5mag down the PN luminosity function (PNLF). Adopting a foreground extinction of E(B-V)=0.1, we derive a distance to the galaxy of 3.5+/-0.2Mpc, in excellent agreement with the surface brightness fluctuation method. No population effect on the bright cutoff of PNLF is observed in the isophotal radius range of 2-16kpc, but the luminosity specific PN density ({alpha}_2.5_) seems to increase with radius inside of 7kpc, in agreement with the {alpha}_2.5_-color relation observed for other galaxies.
- ID:
- ivo://CDS.VizieR/J/ApJ/855/107
- Title:
- PMAS Integral-field SN hosts COmpilation (PISCO)
- Short Name:
- J/ApJ/855/107
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the PMAS/PPak Integral-field Supernova hosts COmpilation (PISCO), which comprises integral field spectroscopy (IFS) of 232 supernova (SN) host galaxies that hosted 272 SNe, observed over several semesters with the 3.5m telescope at the Calar Alto Observatory (CAHA). PISCO is the largest collection of SN host galaxies observed with wide-field IFS, totaling 466347 individual spectra covering a typical spatial resolution of ~380pc. Focused studies regarding specific SN Ia-related topics will be published elsewhere; this paper aims to present the properties of the SN environments, using stellar population (SP) synthesis, and the gas-phase interstellar medium, providing additional results separating stripped-envelope SNe into their subtypes. With 11270 HII regions detected in all galaxies, we present for the first time a statistical analysis of HII regions, which puts HII regions that have hosted SNe in context with all other star-forming clumps within their galaxies. SNe Ic are associated with environments that are more metal-rich and have higher EW(H{alpha}) and higher star formation rate within their host galaxies than the mean of all HII regions detected within each host. This in contrast to SNe IIb, which occur in environments that are very different compared to other core-collapse SNe types. We find two clear components of young and old SPs at SNe IIn locations. We find that SNe II fast decliners tend to explode at locations where the {Sigma}SFR is more intense. Finally, we outline how a future dedicated IFS survey of galaxies in parallel to an untargeted SN search would overcome the biases in current environmental studies.
- ID:
- ivo://CDS.VizieR/J/ApJ/762/77
- Title:
- PM2GC mass-limited sample surface photometry
- Short Name:
- J/ApJ/762/77
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We search for massive and compact galaxies (superdense galaxies, hereafter SDGs) at z=0.03-0.11 in the Padova-Millennium Galaxy and Group Catalogue (PM2GC), a spectroscopically complete sample representative of the general field population of the local universe. We find that compact galaxies with radii and mass densities comparable to high-z massive and passive galaxies represent 4.4% of all galaxies with stellar masses above 3x10^10^M_{sun}_, yielding a number density of 4.3x10^-4^h^3^/Mpc^3^. Most of them are S0s (70%) or ellipticals (23%), are red, and have intermediate-to-old stellar populations, with a median luminosity-weighted age of 5.4Gyr and a median mass-weighted age of 9.2Gyr. Their velocity dispersions and dynamical masses are consistent with the small radii and high stellar mass estimates. Comparing with the WINGS sample of cluster galaxies at similar redshifts, the fraction of SDGs is three times smaller in the field than in clusters, and cluster SDGs are on average 4Gyr older than field SDGs. We confirm the existence of a universal trend of smaller radii for older luminosity-weighted ages at fixed galaxy mass. As a consequence, the median mass-size relation shifts toward smaller radii for galaxies with older stars, but the effect is much more pronounced in clusters than in the field. Our results show that, on top of the well-known dependence of stellar age on galaxy mass, the luminosity-weighted age of galaxies depends on galaxy compactness at fixed mass and, for a fixed mass and radius, on environment. This effect needs to be taken into account in order not to overestimate the evolution of galaxy sizes from high to low z. Our results and hierarchical simulations suggest that a significant fraction of the massive compact galaxies at high z have evolved into compact galaxies in galaxy clusters today. When stellar age and environmental effects are taken into account, the average amount of size evolution of individual galaxies between high and low z is mild, a factor ~1.6.
- ID:
- ivo://CDS.VizieR/J/A+A/548/A106
- Title:
- PMN J0948+0022 radio-to-gamma-ray monitoring
- Short Name:
- J/A+A/548/A106
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present more than three years of observations at different frequencies, from radio to high-energy gamma-rays, of the Narrow-Line Seyfert 1 (NLS1) Galaxy PMN J0948+0022 (z=0.585). This source is the first NLS1 detected at energies above 100 MeV and therefore can be considered the prototype of this emerging new class of gamma-ray emitting active galactic nuclei (AGN). The observations performed from 2008 August 1 to 2011 December 31 confirmed that PMN J0948+0022 generates a powerful relativistic jet, able to develop an isotropic luminosity at gamma-rays of the order of 10^48^erg/s, at the level of powerful quasars. The evolution of the radiation emission of this source in 2009 and 2010 followed the canonical expectations of relativistic jets, with correlated multiwavelength variability (gamma-rays followed by radio emission after a few months), but it was difficult to retrieve a similar pattern in the light curves of 2011. The comparison of gamma-ray spectra before and including 2011 data suggested that there was a softening of the high-energy spectral slope. We selected five specific epochs to be studied by modelling the broad-band spectrum, characterised by an outburst at gamma-rays or very low/high flux at other wavelengths. The observed variability can largely be explained either by changes in the injected power, the bulk Lorentz factor of the jet or the electron spectrum. The characteristic time scale of doubling/halving flux ranges from a few days to a few months, depending on the frequency and the sampling rate. The shortest doubling time scale at gamma-rays is 2.3+/-0.5days. These small values underline the need of highly-sampled multiwavelength campaigns to better understand the physics of these sources.
- ID:
- ivo://CDS.VizieR/J/A+A/570/A61
- Title:
- PM-selected stars of Hercules galaxy
- Short Name:
- J/A+A/570/A61
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Discovered in the last decade as overdensities of resolved stars, the ultra-faint dwarfs (UFDs) are among the least luminous, most dark-matter dominated, and most metal-poor galaxies known today. They appear as sparse, loose objects with high mass-to-light ratios. Hercules is the prototype of the UFD galaxies. To date, there are still no firm constraints on its total luminosity due to the difficulty of disentangling Hercules bona-fide stars from the severe Galactic field contamination. To better constrain Hercules properties, we aim at removing foreground and background contaminants in the galaxy field using the proper motions of the Milky Way stars and the colour-colour diagram. We have obtained images of Hercules in the r_Sloan_ , B_Bessel_ and U_spec_ bands with the Large Binocular Telescope (LBT) and LBC-BIN mode capabilities. The r_Sloan_ new dataset combined with data from the LBT archive span a time baseline of about 5yr, allowing us to measure proper motions of stars in the Hercules direction for the first time. The U_spec_ data along with existing LBT photometry allowed us to use colour-colour diagram to further remove the field contamination. Description: The Hercules ultra-faint dwarf (UFD) galaxy (J2000 position 16:31:02.0+12:47:25.6) was observed with the Large Binocular Camera (LBC) at the LBT located on Mount Graham in Arizona. The LBC is a wide field imager (4 CCDs, 2Kx4.5K pixels each) with a FoV of ~23'x 23' and a resolution of 0.225"/pix. We employed both archival and proprietary data to have the longest available time baseline. File table2 contains the final catalogue of 528 PM-selected sources. From left to right we report: the source identity (Col. 1), right ascension and declination (Col. 2-3), U_spec_, B_Bessel_ and r_Sloan_ magnitudes with their uncertainty (Col. 4-6), displacement with its uncertainty (Col. 7)
- ID:
- ivo://CDS.VizieR/J/A+A/495/447
- Title:
- PN and HII regions in NGC6822
- Short Name:
- J/A+A/495/447
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Images obtained with the CTIO 4-m telescope and the MOSAIC-2 wide field camera in [OIII] 5007 and Halpha on-band and off-band filters are analyzed to search for emission line objects in the dwarf galaxy NGC 6822. In particular we search for planetary nebula (PN) candidates. In addition, imaging and spectroscopy of a sub-sample of objects obtained with the ESO VLT and FORS 2 spectrograph are used to calibrate the MOSAIC imaging. In the continuum-subtracted images, a large number of line emission regions were detected, for which we measured instrumental magnitudes in all the filters. The [OIII] 5007 and Halpha+[NII] magnitudes were calibrated with the spectroscopy.
2899. PNe in 5 nearby galaxies
- ID:
- ivo://CDS.VizieR/J/ApJ/703/894
- Title:
- PNe in 5 nearby galaxies
- Short Name:
- J/ApJ/703/894
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- As the second step in our investigation of the mass-to-light ratio of spiral disks, we present the results of a spectroscopic survey of planetary nebulae (PNe) in five nearby, low-inclination galaxies: IC 342, M74 (NGC 628), M83 (NGC 5236), M94 (NGC 4736), and M101 (NGC 5457). Using 50 setups of the WIYN/Hydra and Blanco/Hydra spectrographs, and 25 observations with the Hobby-Eberly Telescope's Medium Resolution Spectrograph, we determine the radial velocities of 99, 102, 162, 127, and 48 PNe, respectively, to a precision better than 15km/s. Although the main purpose of this data set is to facilitate dynamical mass measurements throughout the inner and outer disks of large spiral galaxies, our spectroscopy has other uses as well. Here, we co-add these spectra to show that, to first order, the [OIII] and Balmer line ratios of PNe vary little over the top ~1.5mag of the PN luminosity function.
2900. PNe in six galaxies
- ID:
- ivo://CDS.VizieR/J/ApJ/577/31
- Title:
- PNe in six galaxies
- Short Name:
- J/ApJ/577/31
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the results of [O III] {lambda}5007 surveys for planetary nebulae (PNe) in six galaxies: NGC 2403, NGC 3115, NGC 3351, NGC 3627, NGC 4258, and NGC 5866. Using on-band/off-band [O III] {lambda}5007 images, as well as images taken in H{alpha}, we identify samples of PNe in these galaxies and derive their distances using the planetary nebula luminosity function (PNLF).
