The planetary nebula population in the halo of M 87

Longobardi, A.; Arnaboldi, M.; Gerhard, Ortwin; Coccato, L.; Okamura, S.; Freeman, K. C.

doi:10.1051/0004-6361/201321652

Cited by 63 publications

(166 citation statements)

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“…2 The transformation between the AB and 5007 magnitudes for the photometric narrowband filter is given by m 5007 = m AB + 2.49 (Longobardi et al 2013). (Mihos et al 2005) with the positions of the FLAMES fields studied in this work (cyan circles) and in previous surveys (dotted black circles) by Arnaboldi et al (2004) and Doherty et al (2009).…”

Section: Observations and Data Reductionmentioning

confidence: 98%

“…(Mihos et al 2005) with the positions of the FLAMES fields studied in this work (cyan circles) and in previous surveys (dotted black circles) by Arnaboldi et al (2004) and Doherty et al (2009). Black squares represent the SuprimeCam survey fields used for the extraction of the photometric PN candidates (Longobardi et al 2013). Bottom panel: schematic zoom-in of the surveyed area (black rectangles).…”

Section: Observations and Data Reductionmentioning

confidence: 98%

“…The photometric candidates targeted by our spectroscopic survey come from an earlier imaging survey (Longobardi et al 2013), covering a 0.43 deg 2 region centred on M 87. Images were taken through a narrowband filter centred on the redshifted [OIII]λ5007 Å emission line at the Virgo cluster distance (onband image), and through a broadband V-filter (off-band image).…”

Section: Photometric Samplementioning

confidence: 99%

“…In this procedure, the PN candidates were selected using automatic selection criteria, based on the distribution of the detected sources in the colour-magnitude (CM) diagram and the properties of their point-spread function (PSF; for more details see Arnaboldi et al 2002;Longobardi et al 2013). This automatic catalogue is complete within the magnitude range 26.3 ≤ m 5007 ≤ 28.4.…”

Section: Photometric Samplementioning

confidence: 99%

“…Bottom panel: schematic zoom-in of the surveyed area (black rectangles). FLAMES pointings (cyan circles) and PN candidates from the photometric survey (black asterisks; Longobardi et al 2013) are plotted over the isophotes of the M 87 halo surface brightness (Kormendy et al 2009). The green cross depicts M 87's centre.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

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The outer regions of the giant Virgo galaxy M 87 Kinematic separation of stellar halo and intracluster light

Longobardi

Arnaboldi

Gerhard

et al. 2015

A&A

144

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Aims. We present a spectroscopic study of a sample of 287 planetary nebulas (PNs) around the brightest cluster galaxy (BCG) M 87 in Virgo A, of which 211 are located between 40 kpc and 150 kpc from the galaxy centre. With these data we can distinguish the stellar halo from the co-spatial intracluster light (ICL) and study both components separately. Methods. We obtained PN velocities with a high resolution FLAMES/VLT survey targeting eight fields in a total area of ∼0.4 deg 2 . We identified PNs from their narrow and symmetric redshifted λ5007 Å [OIII] emission line, the presence of the second λ4959 Å [OIII] emission line, and the absence of significant continuum. We implement a robust technique to measure the halo velocity dispersion from the projected phase-space to identify PNs associated with the M 87 halo and ICL. Using photometric magnitudes, we construct PN luminosity functions (PNLFs), which are complete down to m 5007 = 28.8. Results. The velocity distribution of the spectroscopically confirmed PNs is bimodal, containing a narrow component centred on the systemic velocity of the BCG and an off-centred broader component, which we identify as halo and ICL, respectively. We find that 243 PNs are part of the velocity distribution of the M 87 halo, while the remaining subsample of 44 PNs are intracluster PNs (ICPNs). Halo and ICPNs have different spatial distributions: the number density of halo PNs follow the galaxy's surface brightness profile, whereas the ICPNs are characterised by a shallower power-law profile, I ICL ∝ R γ with γ in the range [−0.34, −0.04]. No evidence is found for an asymmetry in the halo and ICPN density distributions when the NW and SE fields are studied separately. A study of the composite PN number density profile confirms the superposition of different PN populations associated with the M 87 halo and the ICL, characterised by different PN specific numbers α. We derive α halo = 1.06 × 10 −8 N PN L −1 ,bol and α ICL = 2.72 × 10 −8 N PN L −1 ,bol , respectively. The M 87 halo PNLF has fewer bright PNs and a steeper slope towards faint magnitudes than the ICPNLF, and both are steeper than the standard PNLF for the M 31 bulge. Moreover, the ICPNLF has a dip at ∼1−1.5 mag fainter than the bright cut-off, reminiscent of the PNLFs of systems with extended star formation history, such as M 33 or the Magellanic clouds. Conclusions. The BCG halo of M 87 and the Virgo ICL are dynamically distinct components with different density profiles and velocity distributions. Moreover, the different α-parameter values and PNLF shapes of the halo and ICL indicate distinct parent stellar populations, consistent with the existence of a gradient towards bluer colours at large radii. These results reflect the hierarchical build-up of the Virgo cluster.

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Section: Observations and Data Reductionmentioning

confidence: 98%

Section: Observations and Data Reductionmentioning

confidence: 98%

Section: Photometric Samplementioning

confidence: 99%

Section: Photometric Samplementioning

confidence: 99%

Section: Observations and Data Reductionmentioning

confidence: 99%

See 3 more Smart Citations

The outer regions of the giant Virgo galaxy M 87 Kinematic separation of stellar halo and intracluster light

Longobardi

Arnaboldi

Gerhard

et al. 2015

A&A

144

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Lessons from the Local Group

Freeman¹,

Elmegreen²,

Block³

et al. 2015

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The Planetary Nebulae Populations in the Local Group

Arnaboldi

2014

Lessons From the Local Group

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Planetary nebulae have been used as tracers of light and kinematics for the stellar populations in early-type galaxies since more than twenty years. Several empirical properties have surfaced: for example the invariant bright cut-off of the planetary nebulae luminosity function and correlations of the luminosity specific PN number with the integrated properties of the parent stellar populations. These observed properties are poorly understood in terms of a simple model of a ionized nebula expanding around an non-evolving central star. In order to make further steps, we need to study self-contained systems at know distances whose PN populations are sufficiently nearby to permit investigation into their physical properties. The galaxies in the Local Group represent a valid proxies to study these late phases of evolved stellar populations with a spread of metallicities, α-element enhancements, and star forming histories.

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The planetary nebula population in the halo of M 87

Cited by 63 publications

References 56 publications

The outer regions of the giant Virgo galaxy M 87 Kinematic separation of stellar halo and intracluster light

The outer regions of the giant Virgo galaxy M 87 Kinematic separation of stellar halo and intracluster light

Lessons from the Local Group

The Planetary Nebulae Populations in the Local Group

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