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Author: marlageha

mk_table1.ipynb

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+#! /usr/bin/python
+##################################################
+#  COMPILE SPECTRA FROM ALL SOURCES FOR ALL FLAG 0 HOSTS
+#       1. SDSS 
+# 		2. GAMA
+#       3. MMT, AAT, IMACS, WIYN 
+#
+#
+#
+##################################################
+
+import numpy as np
+import os
+
+import matplotlib.pyplot as plt
+from scipy import integrate
+
+
+from astropy import table
+from astropy.table import Table
+from astropy import units as u
+from astropy.io import ascii
+
+
+
+from astroML.plotting import setup_text_plots
+setup_text_plots(fontsize=9, usetex=True)
+
+
+from utils import get_mcconn_table
+from palettable.colorbrewer.qualitative import Dark2_8
+
+
+SAGA_DIR   = os.environ['SAGA_DIR']
+
+############################################################################
+def plot_mwsats():
+
+	if 'plt' in locals() and hasattr(plt, 'rcParams'):
+		plt.rcParams['lines.linewidth'] = 2.5
+		plt.rcParams['font.size'] = 18.0
+		plt.rcParams['font.family'] = 'serif'
+		plt.rcParams['axes.prop_cycle'] = plt.cycler(color=Dark2_8.mpl_colors)
+		plt.rcParams['legend.fontsize'] = 'medium'
+		plt.rcParams['legend.frameon'] = False
+		plt.rcParams['figure.dpi'] = 100
+		plt.rcParams['figure.figsize'] = 7, 6
+		plt.rcParams['xtick.major.size'] = 6
+		plt.rcParams['xtick.minor.size'] = 4
+		plt.rcParams['ytick.major.size'] = 6
+		plt.rcParams['ytick.minor.size'] = 4
+
+
+	# READ SPECTRA
+	file = SAGA_DIR +'/data/saga_spectra_clean.fits.gz'
+	allspec = Table.read(file)
+
+
+
+	m1 = allspec['SATS'] == 1
+	m2 = allspec['TELNAME'] != 'SDSS'
+	m3 = allspec['TELNAME'] != 'NSA'
+	m4 = allspec['TELNAME'] != 'GAMA'
+	m5 = allspec['HOST_SAGA_NAME'] != ''
+	sdss_sats = allspec[m1&m5]
+
+
+
+   # MCCONNACHIE DATA
+	mcconndat = get_mcconn_table()
+
+	# CALCULATE NUMBER OF MW SATS
+	mcconndat.columns
+	mw = mcconndat['distance']<300
+	MV = mcconndat['Vmag'] - mcconndat['distmod'] - 0.3
+	msk = MV < -12.3
+	msk = MV < -7
+	print "brighter than -12"
+	print mcconndat['name'][msk&mw],MV[msk&mw]
+
+	print "brighter than -10"
+	msk = MV < -10.5
+	print mcconndat['name'][msk&mw],MV[msk&mw]
+
+
+	for obj in mcconndat[msk&mw]:#
+		MV = obj['Vmag'] - obj['distmod'] - 0.3
+		print obj['name'],MV,obj['muV0']-0.3
+
+	sample = mcconndat['distance']<0
+	sample[mcconndat['name']=='LMC'] = True
+	sample[mcconndat['name']=='SMC'] = True
+	sample[mcconndat['name']=='Sagittarius'] = True
+	sample[mcconndat['name']=='Fornax'] = True
+	sample[mcconndat['name']=='Leo I'] = True
+	sample[mcconndat['name']=='Sculptor'] = True
+	sample[mcconndat['name']=='M32'] = True
+
+
+	ldat = mcconndat[sample]
+
+
+
+
+
+	sagadists = [5, 20, 30, 40] * u.Mpc
+	distmods = 5*np.log10(sagadists/(10*u.pc))
+
+	data = ldat[ldat['Vabs']<-10]
+	data = data[np.argsort(data['Vabs'])]
+
+
+
+	# UPDATE LMC/SMC
+	m = data['name'] == 'LMC'
+	data['rh_phys'][m] = 2.2   # Bothun & thompson 1988
+	m = data['name'] == 'SMC'
+	data['rh_phys'][m] = 1.0
+
+
+	fig = plt.figure(figsize=(7, 3))
+	plt.rcParams['font.size'] = 18.0
+
+	fig.subplots_adjust(bottom=0.15, top=0.9,left=0.12, right=0.95, wspace=0.3)
+
+	cc = ['red','orange','brown','yellow','green','blue']
+
+
+    # PLOT SIZES
+	plt.subplot(1,2,1)
+	plt.plot(sdss_sats['HOST_DIST'],sdss_sats['PETRORAD_R'],'.',color='grey',label='SAGA sats')
+	for i,gal in enumerate(data):
+		plt.plot(sagadists.value, ((gal['rh_phys']/sagadists.to(u.kpc).value)*u.rad).to(u.arcsec).value,'-o',c=cc[i],label=gal['name'])
+		print ((gal['rh_phys']/sagadists.to(u.kpc).value)*u.rad).to(u.arcsec).value
+
+	plt.ylim(0,25)
+	plt.xlim(18,42)
+	plt.xlabel('Dist [Mpc]')
+	plt.ylabel('$r_{\mathrm{eff}}$ [arcsec]')
+
+	plt.axhline(1., c='k', ls='--')
+
+    # PLOT SAGA DATA
+
+	######################	
+	plt.subplot(1,2,2)
+
+
+	Vmr=0.3
+	rad = 3*u.arcsec/2. #3" diam = fibermag
+
+	for n in data:
+		print n['name'],n['Vabs']-Vmr
+
+
+	  # PLOT SAGA DATA
+	plt.plot(sdss_sats['FIBERMAG_R'],sdss_sats['r'] - sdss_sats['EXTINCTION_R'],'.',color='grey',label='SAGA sats')
+
+
+
+	#first do plummer
+	for i, gal in enumerate(data):
+	    fracs = np.array([frac_inside(gal, rad, dist, 'plummer') for dist in sagadists])
+	    fibmags = gal_mag_frac(gal, fracs, sagadists) - Vmr
+	    totmags = gal_mag_frac(gal, np.ones_like(fracs), sagadists) - Vmr
+	    
+#	    plt.plot(fibmags, totmags,'-o',color=cc[i],label=gal['name'])
+	    
+#	        plt.text(fibmags[fi], totmags[ti], gal['name'],color=cc[i])
+	#plt.legend(loc=0)
+
+
+
+
+
+	for i, gal in enumerate(data):
+	    fracs = np.array([frac_inside(gal, rad, dist, 'exp') for dist in sagadists])
+	    fibmags = gal_mag_frac(gal, fracs, sagadists) - Vmr
+	    totmags = gal_mag_frac(gal, np.ones_like(fracs), sagadists) - Vmr
+	    
+	    plt.plot(fibmags, totmags,'-o',color=cc[i],label=gal['name'])
+
+	plt.legend(loc=2,fontsize=7)
+	    
+#	x1t1 = [min(fiblim[0], totlim[0]), max(fiblim[1], totlim[1])]
+#	plt.fill_between(x1t1,x1t1, totlim[1],facecolor=[0.6]*3)
+	plt.axhline(20.75, c='k', ls=':')
+	plt.axvline(23, c='k', ls=':')
+
+
+	    
+	plt.xlabel('Fibermag\_r')
+	plt.ylabel('$r_o$')
+#	plt.title('Solid=Plummer, Dashed=Exponential')
+	plt.xlim(14.5,23.5) #tweak for text
+	plt.ylim(12,22.)
+
+
+
+
+
+
+	plt.show()
+	plt.savefig('fig_mwsats.pdf')
+
+def plummer_prof(r, totflux=1, Reff=1):
+	a = Reff*(2.**(2./3)-1.)**(-0.5)
+	return 2*a*(3 * totflux / (4*np.pi*a**3))*(1+(r/a)**2)**-2.5
+
+
+def exp_prof(r, totflux=1, Reff=1):
+    from scipy.special import lambertw
+    #the parenthetical below is non-trivial, but it's ~1.67835
+    rs = Reff / -(lambertw(-1/2/np.exp(1),-1).real+1.)
+    rs = Reff/1.67835
+#    print rs
+    return totflux*np.exp(-r/rs)/np.pi/2./rs/rs
+
+
+def frac_inside(gal, radius, dist, prof):
+    """
+    Compute the magnitude inside the given angular `radius` for the
+    table entry `gal` at a distance of `dist`, assuming a profile
+    `prof` ('plummer' or 'exp')
+    """    
+    if prof == 'plummer':
+        prof_func = plummer_prof
+    elif prof == 'exp':
+        prof_func = exp_prof
+    else:
+        raise ValueError('invalid profile type '+ str(prof))
+        
+    rh_at_distance = (u.arcmin*gal['rh'] * (gal['distance']*u.kpc)/dist).to(u.arcmin)
+    return integrate.quad(lambda x:prof_func(x, 1, rh_at_distance.value)*x*np.pi*2, 0, radius.to(u.arcmin).value)[0]
+
+def gal_mag_frac(gal, frac, dist):
+    """
+    determine the V magnitude for `frac` of the flux from `gal` at distance `dist`
+    """
+    flux = 10**((gal['Vabs'])/-2.5)
+    fluxd = flux * ((10*u.pc/dist)**2).decompose().value
+    return -2.5*np.log10(frac*fluxd)
+
+
+
+if __name__ == '__main__':
+    create_saga_spectra()
+
+ 
+
+