scholarly journals A Database of Cepheid Distance Moduli and Tip of the Red Giant Branch, Globular Cluster Luminosity Function, Planetary Nebula Luminosity Function, and Surface Brightness Fluctuation Data Useful for Distance Determinations

2000 ◽  
Vol 128 (2) ◽  
pp. 431-459 ◽  
Author(s):  
Laura Ferrarese, ◽  
Holland C. Ford ◽  
John Huchra ◽  
Robert C. Kennicutt, Jr. ◽  
Jeremy R. Mould ◽  
...  
Keyword(s):  
Globular Cluster ◽  
Planetary Nebula ◽  
Surface Brightness ◽  
Luminosity Function ◽  
Brightness Fluctuation ◽  
Red Giant

scholarly journals New Insights from a Study of the Globular Cluster Systems of 60 Early-Type Galaxies

2002 ◽  
Vol 207 ◽  
pp. 229-237
Author(s):  
Arunav Kundu ◽  
Brad Whitmore
Keyword(s):  
Globular Cluster ◽  
Surface Brightness ◽  
Luminosity Function ◽  
Photometric Study ◽  
Early Type ◽  
Color Distribution ◽  
Cluster Systems ◽  
Brightness Fluctuation ◽  
Distance Indicator ◽  
Fluctuation Method

We present the results of our detailed WFPC2-based photometric study of the globular cluster systems (GCS) of over 60 elliptical and SO galaxies. Approximately 50% of the GCSs of ellipticals, and at least 15–20% of S0s reveal bimodality in the color distribution. We trace the variation in GCS properties with Hubble type and discuss the implications on the various models of galaxy (and cluster system) formation. We also provide evidence that the globular cluster luminosity function is an excellent distance indicator with an accuracy comparable to the surface brightness fluctuation method.

scholarly journals The planetary nebula luminosity function

2012 ◽  
Vol 8 (S289) ◽  
pp. 247-254
Author(s):  
Robin Ciardullo
Keyword(s):  
Planetary Nebula ◽  
Surface Brightness ◽  
Luminosity Function ◽  
Zero Point ◽  
Theoretical Explanation ◽  
Number Of Factors ◽  
Surface Brightness Fluctuations ◽  
Type Ia ◽  
Red Giant ◽  
Supernovae Type Ia

AbstractAlthough the method has no theoretical explanation, the [Oiii]λ5007Å planetary nebula luminosity function (PNLF) is an extremely valuable tool for obtaining accurate (< 10%) extragalactic distances out to ~ 18 Mpc. Because the PNLF works in large galaxies of all Hubble types, it is one of the best tools we have for cross-checking the results of other methods and identifying systematic offsets between the Population I and Population II distance ladders. We review the PNLF's calibration and show that the method's Cepheid-derived zero point is virtually identical to that inferred from measurements of the tip of the red giant branch. We then compare the PNLF to the surface brightness fluctuations method and demonstrate that the latter's calibration yields a distance scale that is ~ 15% larger than that of the PNLF. We argue that this offset is likely due to a number of factors, including the effects of reddening on both of the techniques. We conclude by discussing the use of the PNLF for supernovae Type Ia calibration and considering the outstanding problems associated with the method.

scholarly journals Calibration of Surface Brightness Fluctuations for Dwarf Galaxies in the Hyper Suprime-Cam gi Filter System

2021 ◽  
Vol 923 (2) ◽  
pp. 152
Author(s):  
Yoo Jung Kim ◽  
Myung Gyoon Lee
Keyword(s):  
Surface Brightness ◽  
Stellar Population ◽  
Dwarf Galaxies ◽  
Imaging Data ◽  
Standard Candle ◽  
Surface Brightness Fluctuations ◽  
Brightness Fluctuation ◽  
Linear Fit ◽  
Red Giant ◽  
Red Galaxies

Abstract Surface brightness fluctuation (SBF) magnitudes are a powerful standard candle to measure distances to semiresolved galaxies in the local universe, a majority of which are dwarf galaxies that often have bluer colors than bright early-type galaxies. We present an empirical i-band SBF calibration in a blue regime, 0.2 ≲ (g − i)0 ≲ 0.8 in the Hyper Suprime-Cam (HSC) magnitude system. We measure SBF magnitudes for 12 nearby dwarf galaxies of various morphological types with archival HSC imaging data, and use their tip of the red giant branch distances to derive fluctuation–color relations. In order to subtract contributions of fluctuations due to young stellar populations, we use five different g-band magnitude masking thresholds, M g,thres = −3.5, −4.0, −4.5, −5.0, and −5.5 mag. We find that the rms scatter of the linear fit to the relation is the smallest (rms = 0.16 mag) in the case of M g,thres = −4.0 mag, M ¯ i = (−2.65 ± 0.13) + (1.28 ± 0.24) × (g − i)0. This scatter is much smaller than those in the previous studies (rms = 0.26 mag), and is closer to the value for bright red galaxies (rms = 0.12 mag). This calibration is consistent with predictions from metal-poor simple stellar population models.

scholarly journals Securing the Faint End of the Galaxy Luminosity Function

2004 ◽  
Vol 21 (4) ◽  
pp. 356-359 ◽  
Author(s):  
Helmut Jerjen ◽  
Brent Tully ◽  
Neil Trentham
Keyword(s):  
Surface Brightness ◽  
Luminosity Function ◽  
Dwarf Galaxy ◽  
Full Range ◽  
Mass Function ◽  
Wide Field ◽  
Distance Information ◽  
The Galaxy ◽  
Brightness Fluctuation ◽  
Galaxy Luminosity Function

AbstractThe history of the formation of galaxies must leave an imprint in the properties of the mass function of collapsed objects and in its observational manifestation, the galaxy luminosity function. At present the faint end of the luminosity function is poorly known. Accurate knowledge of the luminosity function over the full range of galaxy clustering scales would provide serious constraints on both initial cosmological conditions and modulating astrophysical processes.Wide field imaging surveys with large ground-based telescopes now provide the capability to identify dwarf galaxy candidates to very faint levels (μR ≈ 26 mag arcsec–2), too low in surface brightness for spectroscopy (measuring redshifts) even with telescopes like Keck. Other means have to be explored to get distance information for these candidates in order to separate cluster members from back/foreground systems beyond doubt. On the quest to establish the properties (slope and possible turning point) of the the faint end of the galaxy luminosity function we are employing the surface brightness fluctuation (SBF) method to determine adequate distances, potentially resulting in the best definition ever of the luminosity function to MR ≈ –11 in the cluster and group environments.

scholarly journals KKH 22, the first dwarf spheroidal satellite of IC 342

2020 ◽  
Vol 638 ◽  
pp. A111
Author(s):  
Igor D. Karachentsev ◽  
Lidia N. Makarova ◽  
R. Brent Tully ◽  
Gagandeep S. Anand ◽  
Luca Rizzi ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Spiral Galaxy ◽  
Globular Cluster ◽  
Surface Brightness ◽  
Absolute Magnitude ◽  
Peculiar Velocity ◽  
Central Surface ◽  
Red Giant ◽  
Advanced Camera For Surveys ◽  
Heliocentric Velocity

Aims. We present observations with the Advanced Camera for Surveys on the Hubble Space Telescope of the nearby dwarf spheroidal galaxy KKH 22 = LEDA 2807114 in the vicinity of the massive spiral galaxy IC 342. Methods. We derived its distance of 3.12 ± 0.19 Mpc using the tip of red giant branch (TRGB) method. We also used the 6 m BTA spectroscopy to measure a heliocentric radial velocity of the globular cluster in KKH 22 to be +30 ± 10 km s−1. Results. The dSph galaxy KKH 22 has the V-band absolute magnitude of –12.m19 and the central surface brightness μv, 0 = 24.1m/□″. Both the velocity and the distance of KKH 22 are consistent with the dSph galaxy being gravitationally bound to IC 342. Another nearby dIr galaxy, KKH 34, with a low heliocentric velocity of +106 km s−1 has the TRGB distance of 7.28 ± 0.36 Mpc residing in the background with respect to the IC 342 group. KKH 34 has a surprisingly high negative peculiar velocity of –236 ± 26 km s−1.

scholarly journals The Planetary Nebulae Luminosity Function (PNLF): current perspectives

2016 ◽  
Vol 12 (S323) ◽  
pp. 298-302 ◽  
Author(s):  
Roberto H. Méndez
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Method ◽  
Surface Brightness ◽  
Luminosity Function ◽  
Recent Progress ◽  
Historical Review ◽  
Stellar Populations ◽  
Surface Brightness Fluctuations ◽  
Distance Indicator ◽  
Red Giant

AbstractThis paper starts with a brief historical review about the PNLF and its use as a distance indicator. Then the PNLF distances are compared with Surface Brightness Fluctuations (SBF) distances and Tip of the Red Giant Branch (TRGB) distances. A Monte Carlo method to generate simulated PNLFs is described, leading to the last subject: recent progress in reproducing the expected maximum final mass in old stellar populations, a stellar astrophysics enigma that has been challenging us for quite some time.

Planetary Nebulae as Extragalactic Distance Indicators

2003 ◽  
Vol 209 ◽  
pp. 617-624 ◽  
Author(s):  
Robin Ciardullo
Keyword(s):  
Excellent Agreement ◽  
Planetary Nebula ◽  
Surface Brightness ◽  
Luminosity Function ◽  
Planetary Nebulae ◽  
General Purpose ◽  
Distance Scale ◽  
Standard Candle ◽  
Surface Brightness Fluctuations ◽  
Distance Indicators

The planetary nebula luminosity function (PNLF) plays a key role in the distance ladder, as it is the only general purpose standard candle that is applicable to both Pop I and Pop II systems. We review the physics underlying the method, and compare its distances to distances obtained from Cepheids and surface brightness fluctuations (SBF). We show that PNLF distances agree with the geometric distances to the LMC and NGC 4258, and that, on a galaxy-by-galaxy basis, the relative PNLF, Cepheid, and SBF distances are in excellent agreement with no systematic trends. However, even though the PNLF and SBF methods are both calibrated by Cepheids, the PNLF distance scale is ~17% smaller than the SBF scale. We discuss this offset, and examine the possible causes of the discrepancy.

scholarly journals The Distance to NGC 5128 (Centaurus A)

2010 ◽  
Vol 27 (4) ◽  
pp. 457-462 ◽  
Author(s):  
Gretchen L. H. Harris ◽  
Marina Rejkuba ◽  
William E. Harris
Keyword(s):  
Surface Brightness ◽  
Luminosity Function ◽  
Current Data ◽  
Long Period ◽  
Surface Brightness Fluctuations ◽  
Period Variable ◽  
Red Giant ◽  
Extragalactic Distance Scale ◽  
Centaurus A

AbstractIn this paper we review the various high precision methods that are now available to determine the distance to NGC 5128. These methods include: Cepheids, TRGB (tip of the red giant branch), PNLF (planetary nebula luminosity function), SBF (surface brightness fluctuations), and Long Period Variable (LPV) Mira stars. From an evaluation of these methods and their uncertainties, we derive a best-estimate distance of 3.8±0.1 Mpc to NGC 5128 and find that this mean is now well supported by the current data. We also discuss the role of NGC 5128 more generally for the extragalactic distance scale as a testbed for the most direct possible comparison among these key methods.

scholarly journals Near Infrared Photometry of New Galactic Globular Clusters GC 01 and GC 02

2002 ◽  
Vol 207 ◽  
pp. 107-109 ◽  
Author(s):  
J. Borissova ◽  
V. D. Ivanov ◽  
L. Vanzi
Keyword(s):  
Globular Cluster ◽  
Preliminary Report ◽  
Globular Clusters ◽  
Surface Brightness ◽  
Near Infrared ◽  
Infrared Photometry ◽  
Galactic Globular Clusters ◽  
Red Giant ◽  
Best Fit ◽  
Calculated Distance

We present a preliminary report on the first deep near infrared photometry of 2MASS GC 01 and 2MASS GC 02 - new Galactic globular cluster candidates, discovered by the 2MASS. The red giant branch slopes yielded [Fe/H]=-0.42 ± 0.15 dex and [Fe/H]=-0.66 ± 0.17 dex, respectively for GC 01 and GC 02. We estimated the reddening towards GC 01 and GC 02: E(B - V) = 5.36 ± 0.20, and E(B - V) = 4.55 ± 0.17. The calculated distance moduli to the clusters are: (m - M)0 = 13.53 ± 0.27 and (m - M)0 = 14.53 ± 0.31 for GC 01 and GC 02. Our best fit for the radial surface brightness profile of GC 02 yields: lg(rc) = 1.40, lg(rh) = 1.54, lg(rt) = 1.31, and c=1.60. CC 01 is less concentrated: lg(rc) = 1.63, lg(rh) = 1.7, lg(rt) = 1.25, and c=1.41.

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