A Comparison of the Planetary Nebula Luminosity Function and Surface Brightness Fluctuation Distance Scales

1993 ◽  
Vol 419 ◽  
pp. 479 ◽  
Author(s):  
Robin Ciardullo ◽  
George H. Jacoby ◽  
John L. Tonry
Keyword(s):  
Planetary Nebula ◽  
Surface Brightness ◽  
Luminosity Function ◽  
Brightness Fluctuation

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 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 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.

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 Planetary Nebulae in M31: Abundances, and comparison with bright Planetary Nebulae in the LMC

1997 ◽  
Vol 180 ◽  
pp. 475-476
Author(s):  
M. G. Richer ◽  
G. Stasińska ◽  
M. L. McCall
Keyword(s):  
Planetary Nebula ◽  
Luminosity Function ◽  
Large Population ◽  
Wavelength Region ◽  
Planetary Nebulae ◽  
Surprising Result ◽  
Population Synthesis ◽  
Abundance Distribution ◽  
Wide Range ◽  
The Mean

We have obtained spectra of 28 planetary nebulae in the bulge of M31 using the MOS spectrograph at the Canada-France-Hawaii Telescope. Typically, we observed the [O II] λ3727 to He I λ5876 wavelength region at a resolution of approximately 1.6 å/pixel. For 19 of the 21 planetary nebulae whose [OIII]λ5007 luminosities are within 1 mag of the peak of the planetary nebula luminosity function, our oxygen abundances are based upon a measured [OIII]λ4363 intensity, so they are based upon a measured electron temperature. The oxygen abundances cover a wide range, 7.85 dex < 12 + log(O/H) < 9.09 dex, but the mean abundance is surprisingly low, 12 + log(O/H)–8.64 ± 0.32 dex, i.e., roughly half the solar value (Anders & Grevesse 1989). The distribution of oxygen abundances is shown in Figure 1, where the ordinate indicates the number of planetary nebulae with abundances within ±0.1 dex of any point on the x-axis. The dashed line indicates the mean abundance, and the dotted lines indicate the ±1 σ points. The shape of this abundance distribution seems to indicate that the bulge of M31 does not contain a large population of bright, oxygen-rich planetary nebulae. This is a surprising result, for various population synthesis studies (e.g., Bica et al. 1990) have found a mean stellar metallicity approximately 0.2 dex above solar. This 0.5 dex discrepancy leads one to question whether the mean stellar metallicity is as high as the population synthesis results indicate or if such metal-rich stars produce bright planetary nebulae at all. This could be a clue concerning the mechanism responsible for the variation in the number of bright planetary nebulae observed per unit luminosity in different galaxies (e.g., Hui et al. 1993).

scholarly journals Calibrating Type Ia Supernovae Using the Planetary Nebula Luminosity Function. I. Initial Results

2007 ◽  
Vol 657 (1) ◽  
pp. 76-94 ◽  
Author(s):  
John J. Feldmeier ◽  
George H. Jacoby ◽  
M. M. Phillips
Keyword(s):  
Planetary Nebula ◽  
Luminosity Function ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Ia Supernovae ◽  
Initial Results

scholarly journals A two-mode planetary nebula luminosity function

2015 ◽  
Vol 575 ◽  
pp. A1 ◽  
Author(s):  
A. Rodríguez-González ◽  
L. Hernández-Martínez ◽  
A. Esquivel ◽  
A. C. Raga ◽  
G. Stasińska ◽  
...  
Keyword(s):  
Planetary Nebula ◽  
Luminosity Function

scholarly journals Distance determination to NGC 55 from the planetary nebula luminosity function

2006 ◽  
Vol 455 (3) ◽  
pp. 891-896 ◽  
Author(s):  
G. C. Van de Steene ◽  
G. H. Jacoby ◽  
C. Praet ◽  
R. Ciardullo ◽  
H. Dejonghe
Keyword(s):  
Planetary Nebula ◽  
Luminosity Function ◽  
Distance Determination

scholarly journals Infrared Surface Brightness Fluctuation Distances for MASSIVE and Type Ia Supernova Host Galaxies*

2021 ◽  
Vol 255 (2) ◽  
pp. 21
Author(s):  
Joseph B. Jensen ◽  
John P. Blakeslee ◽  
Chung-Pei Ma ◽  
Peter A. Milne ◽  
Peter J. Brown ◽  
...  
Keyword(s):  
Surface Brightness ◽  
Host Galaxies ◽  
Type Ia Supernova ◽  
Type Ia ◽  
Brightness Fluctuation
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