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Teff [K]:
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log(g):
distance [pc]:
distance [pc]:

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( including unresolved double degenerates)
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Solid lines show ZZ Ceti instability strip (Van Grootel et al. 2013 ADS)
Dotted lines show empirical ZZ Ceti instability strip (Gianninas et al. 2011 ADS)
Dashed lines show V777 Her instability strip (Gilles Fontaine, private communication)

Plot properties

stars in the plot
( including unresolved double degenerates)

DA: DB: CND:
DC: DQ:
DZ: PG1159:
DO: Other:

X axis: 

minus
Flip X axis

Y axis: 

minus
Flip Y axis

Dot radius: 

Dot color: 

X axis limits: 

from: 

to: 

Y axis limits: 

from: 

to: 

Histogram properties

objects used for histogram
( including unresolved double degenerates)

DA: DB: CND:
DC: DQ:
DZ: PG1159:
DO: Other:

X axis: 

X axis limit:
from:
to:
Y axis limit:
from:
to:
Bin width :

Options

objects used for histogram
( including unresolved double degenerates)

X axis limit:
from:
to:
Y axis limit:
from:
to:
Bin width (K):

Sun abundances were taken from Lodders, K. 2003, Solar System Abundances and Condensation Temperatures of the Elements, ADS

Plot properties

stars in the plot

DA: DB: CND:
DC: DQ:
DZ: PG1159:
DO: Other:
X axis:
log( / )
Y axis:
log( / )
Dot radius:
Dot color:
X axis limits:
from:
to:
Y axis limits:
from:
to:

Completeness

Assuming a local white dwarf density of
(pc-3), within pc we expect ~ stars.
Our database contains objects corresponding to %
completeness.
Logarithmic scale





















The Montreal White Dwarf Database is produced and maintained by Prof. Patrick Dufour at Université de Montréal. Please send database updates, corrections, suggestions or bug reports to dufourpa@astro.umontreal.ca.