Mfreq

This table contains properties of galaxy clusters, produced by Zandanel, Pfrommer & Prada 2014a and Zandanel, Pfrommer & Prada 2014b. A short description of the method can be found at Galaxy Clusters.

The galaxy clusters were generated using only distinct halos from the BDMW catalogue of the MDR1 simulation with a total mass (Mtot) above 1014 Msun/h.
For each galaxy cluster, the table stores its generated properties and additionally the corresponding bdmId of the halo to which it belongs.
Note that these catalogues are available only for snapshots corresponding to the redshift values z = 0, 0.05, 0.1, 0.16, 0.18, 0.2, 0.27, 0.32, 0.37, 0.4, 0.47, 0.53, 0.61, 0.69, 0.78, 0.89 and 1.

Column Type UCD Unit Description
galclusterId bigint meta.id; meta.main unique id for the galaxy cluster, = snapnum*106 + NInCat
bdmId bigint meta.id; meta.main bdmId of BDMW table
snapnum int time.epoch number of snapshot (same as in halo catalogues)
NInCat int meta.id number of galaxy cluster in original data file
x real pos.cartesian.x 1/h Mpc (comoving) position, x-component
y real pos.cartesian.y 1/h Mpc (comoving) position, y-component
z real pos.cartesian.z 1/h Mpc (comoving) position, z-component
vx real phys.veloc; pos.cartesian.x km/s (peculiar) velocity, x-component
vy real phys.veloc; pos.cartesian.y km/s (peculiar) velocity, y-component
vz real phys.veloc; pos.cartesian.z km/s (peculiar) velocity, z-component
np int meta.number number of particles in halo
Mvir real phys.mass 1/h Msun halo mass – mass of bound particles within Rvir
Mtot real phys.mass 1/h Msun halo mass – mass of all particles within Rvir
Rvir real phys.size.radius 1/h Mpc virial radius
M500 real phys.mass 1/h Msun halo mass, defined with 500 * critical density calculated from BDMW Mtot with Hu & Kravtsov (2003) method
R500 real phys.size.radius 1/h Mpc radius for 500 * critical density boundary
T real phys.temperature keV intra-cluster medium X-ray temperature (kBT) from Mantz et al. (2010) Tci – M500 relation
stateFlag int meta.code flag for cluster dynamical state: 0 = non-cool core cluster, 1 = cool-core cluster
rho0 real phys.density h1/2 g cm-3 intra-cluster medium central gas density (at R = 0)
LX real phys.luminosity;em.X-ray h-2 erg/s X-ray thermal bremsstrahlung luminosity within R500
YX real phys.mass, phys.temperature, arith.factor h-2.5 Msun keV YX = Mgas * kBT parameter of Kravtsov et al. (2006) within R500, related to the total thermal energy of the ICM
SZ real phys.density, phys.temperature, arith.factor h-2.5 Mpc2 integrated thermal Sunyaev-Zel’dovich Compton-Y parameter (as equation 3 of Battaglia et al. 2011) within R500
radioFlag int meta.code flag for radio-loud ( = 1; 10%) and radio-quiet ( = 0; 90%) clusters
XCR real phys.pressure, arith.ratio ratio of cosmic-ray to thermal pressure volume avarage (<PCR/Pth>) within R500
radioMHz real phys.luminosity;em.radio h-2 erg/s/Hz synchrotron radio halo luminosity at 120 MHz within R500
radioGHz real phys.luminosity;em.radio h-2 erg/s/Hz synchrotron radio halo luminosity at 1.4 GHz within R500
gammaMeV real phys.luminosity;em.gamma h-2 photons/s gamma-ray luminosity above 100 MeV within R500
gammaGeV real phys.luminosity;em.gamma h-2 photons/s gamma-ray luminosity above 100 GeV within R500
ix int pos.cartesian.x spatial index, x-direction
iy int pos.cartesian.y spatial index, y-direction
iz int pos.cartesian.z spatial index, z-direction
phkey int Peano-Hilbert-key, i.e. index along the Peano-Hilbert curve

Examples

Get the 10 most luminous galaxy clusters (in range above 100 GeV) at z=0 (snapnum 85)

SELECT * FROM MDR1.BDMWMfreq WHERE snapnum=85
ORDER BY gammaGeV DESC
LIMIT 10

This query retrieves the first 10 records from the galaxy cluster-table after sorting them by the gammaGeV-luminosity and hence returns the most luminous objects.

Get the spin of galaxy clusters with gammay ray luminosity above 100 GEV, > 1040 h-2 photons/s

SELECT f.gammaGeV, b.spin FROM MDR1.BDMWMfreq f, MDR1.BDMW b 
WHERE f.bdmId = b.bdmId 
AND f.gammaGeV > 1.e40

By joining the galaxy cluster table with the BDMW table (using the bdmId), one can get access to all properties of the underlying dark matter halos.

Examples for reproducing the figures in Zandanel, Pfrommer & Prada 2013a and Zandanel, Pfrommer & Prada 2013b

The following example queries can be used to reproduce some of the figures in the papers given above.
For those figures where one curve per redshift is given, we just picked one redshift (and thus one snapnum) as example in the query.

Paper I, Figure 2, left: Relation between bolometric X ray luminosity and mass (M500)

SELECT 
    LOG10(val.Ez*b.M500/0.7) AS logEzM, 
    LOG10(b.LX/val.Ez/1.e44/0.7/0.7) AS logLX 
FROM 
    MDR1.BDMWMfreq b, 
    (SELECT SQRT(0.3*POWER((1+0.2),3)+0.7) AS Ez FROM MDR1.BDMV LIMIT 1) AS val
WHERE b.snapnum=74

Here we use the trick to first calculate an expression in a subquery and name it val.Ez, so that it can be used in the main query as a parameter. Since PaQu does not support SELECT-statements without the FROM-clause, we added FROM MDR1.BDMV, but it has no real meaning, it’s just to make the syntax appear correct.)
Please note: though MySQL natively supports declaration of variables, PaQu cannot handle this (yet), also multiple statements with one submit are not allowed. Thus, if we want to use variables, we have to be more tricky here.

We could also make it less complicated by replacing the term SQRT(0.3*POWER((1+0.2),3)+0.7) directly by its value 1.103811578:

SELECT 
    LOG10(1.103811578*M500/0.7) AS logEzM,   
    LOG10(LX/1.103811578/1.e44/0.7/0.7) AS logLX 
FROM MDR1.BDMWMfreq
WHERE snapnum=74

Paper I, Figure 2, right: Relation between thermal energy and mass (YX-M500)

SELECT
    LOG10(val.Ez*b.M500/0.7) AS logEzM,
    LOG10(b.YX*val.Ez*POWER(0.7,(-2.5))) AS logYX
FROM
    MDR1.BDMWMfreq b,
    (SELECT SQRT(0.3*POWER((1+0.2),3)+0.7) AS Ez FROM MDR1.BDMV LIMIT 1) AS val
WHERE b.snapnum=74

Paper I, Figure 4, left: YSZ-M relation

SELECT
    LOG10(b.M500/0.7) AS logEzM,
    LOG10(b.SZ*POWER(val.Ez,(-2/3))*POWER(0.7,-2.5)) AS logSZ
FROM
    MDR1.BDMWMfreq AS b
    (SELECT SQRT(0.3*POWER((1+0.2),3)+0.7) AS Ez FROM MDR1.BDMV LIMIT 1) AS val
WHERE snapnum=75

Paper II, Figure 4, left: Radio-to-X-ray scaling relation (L1.4-YX)

SELECT LOG10(LX/0.7/0.7) AS logLX, LOG10(radioGHz/0.7/0.7) AS logradioGHz 
FROM MDR1.BDMWMfreq
WHERE snapnum=74

Paper II, Figure 4, right: Radio-to-SZ scaling relation (L1.4-YSZ)

SELECT LOG10(SZ*POWER(0.7,(-2.5))) AS logSZ, LOG10(radioGHz/0.7/0.7) AS logradioGHz
FROM MDR1.BDMWMfreq
WHERE snapnum=74

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