J/ApJ/772/131 Musket Ball Cluster redshift catalog (Dawson, 2013)
The dynamics of merging clusters: a Monte Carlo solution applied to the
Bullet and Musket Ball Clusters.
Dawson W.A.
<Astrophys. J., 772, 131 (2013)>
=2013ApJ...772..131D 2013ApJ...772..131D
ADC_Keywords: Clusters, galaxy ; Galaxies, optical ; Spectroscopy ; Redshifts
Keywords: galaxies: clusters: individual (1ES 0657-558, DLSCL J0916.2+2951);
gravitation; methods: analytical; methods: statistical
Abstract:
Merging galaxy clusters have become one of the most important probes
of dark matter, providing evidence for dark matter over modified
gravity and even constraints on the dark matter self-interaction
cross-section. To properly constrain the dark matter cross-section it
is necessary to understand the dynamics of the merger, as the inferred
cross-section is a function of both the velocity of the collision and
the observed time since collision. While the best understanding of
merging system dynamics comes from N-body simulations, these are
computationally intensive and often explore only a limited volume of
the merger phase space allowed by observed parameter uncertainty.
Simple analytic models exist but the assumptions of these methods
invalidate their results near the collision time, plus error
propagation of the highly correlated merger parameters is unfeasible.
To address these weaknesses I develop a Monte Carlo method to discern
the properties of dissociative mergers and propagate the uncertainty
of the measured cluster parameters in an accurate and Bayesian manner.
I introduce this method, verify it against an existing hydrodynamic
N-body simulation, and apply it to two known dissociative mergers:
1ES 0657-558 (Bullet Cluster) and DLSCL J0916.2+2951 (Musket Ball
Cluster).
Description:
The Musket Ball Cluster redshift catalog (Table 4) contains 738
spectroscopically confirmed galaxy redshifts. The galaxies are within
an ∼18'x18' area centered on the Musket Ball Cluster (139.05deg,
+29.85deg). The sources of the redshifts are from three separate
spectroscopic surveys: (1) LRIS 2007 was carried out on 2007 January
15 using the Keck:I LRIS instrument, (2) DEIMOS 2011A was carried out
on 2011 March 1 and 2 using the Keck:II DEIMOS instrument
(5400-8000Å), and (3) DEIMOS 2012B was carried out on 2013 January
16 using the Keck:II DEIMOS instrument (4900-7500Å).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 74 738 Musket Ball Cluster redshift catalog
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See also:
J/A+A/540/A43 : New redshifts for Abell 1758N galaxies (Boschin+, 2012)
J/ApJS/188/280 : Spectroscopic catalog in 24 clusters (Stern+, 2010)
J/MNRAS/406/1318 : Lensed-arc statistics of galaxy clusters (Horesh+, 2010)
J/A+A/503/357 : Redhift catalog of A1237+A1240 galaxies (Barrena+, 2009)
J/A+A/491/379 : Velocities of galaxies in Abell 520 (Girardi+, 2008)
J/AJ/129/31 : A deep radio survey of Abell 2125. II (Owen+, 2005)
J/A+A/430/19 : VRI photometry of Abell 3921 galaxies (Ferrari+, 2005)
J/AJ/125/2427 : 1.4GHz flux densities of Abell 2255 galaxies (Miller+, 2003)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 2 I2 h RAh [9] Hour of Right Ascension (J2000)
4- 5 I2 min RAm [15/16] Minute of Right Ascension (J2000)
7- 12 F6.3 s RAs Second of Right Ascension (J2000)
14 A1 --- DE- [+] Sign of the Declination (J2000)
15- 16 I2 deg DEd [29] Degree of Declination (J2000)
18- 19 I2 arcmin DEm Arcminute of Declination (J2000)
21- 25 F5.2 arcsec DEs Arcsecond of Declination (J2000)
27- 30 F4.2 arcsec ePos [0.5/1.3] Positional uncertainty
32- 39 F8.6 --- z [0.02/1.4] Spectroscopic redshift
41- 48 F8.6 --- e_z [0/5]? Error in z
50- 61 A12 --- r_z Source of z (1)
63- 68 F6.3 mag Rmag [17.9/24.9]? The R band magnitude
70- 74 F5.3 mag e_Rmag [0.001/0.09]? Error in Rmag
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Note (1): Spectroscopic survey as follows:
DEIMOS 2011A = DEIMOS 2011A was carried out on 2011 March 1 and 2 using the
Keck:II DEIMOS instrument. Observations consisted of six slit
masks with 1" slits and using the 1200line/mm grating, tilted
to a central wavelength of 6700Å, resulting in a pixel
scale of 0.33Å/pixel, a resolution of ∼1.1Å (50km/s),
and typical wavelength coverage of 5400Å to 8000Å.
DEIMOS 2011B = DEIMOS 2012B was carried out on 2013 January 16 using the
Keck:II DEIMOS instrument. Observations consisted of 1 slit
mask with 1" slits and using the 1200line/mm grating, tilted
to a central wavelength of 6200Å, resulting in a pixel
scale of 0.33Å/pixel, a resolution of ∼1Å (50km/s), and
typical wavelength coverage of 4900Å to 7500Å.
LRIS 2007 = LRIS 2007 was carried out on 2007 January 15 using the
Keck:I LRIS instrument. Details of the LRIS 2007 observations
and reduction are discussed in the Deep Lens Survey data
release paper (D. Wittman et al., in preparation).
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 04-Feb-2015