  Filaments and coronal holes, two principal features observed in the solar
corona are sources of space weather variations. Filament formation is closely
associated with polarity inversion lines (PIL) on the solar photosphere which
separate positive and negative polarities of the surface magnetic field. The
origin of coronal holes is governed by large-scale unipolar magnetic patches on
the photosphere from where open magnetic field lines extend to the heliosphere.
We study properties of filaments, PILs and coronal holes in solar cycles 20,
21, 22 and 23 utilizing the McIntosh archive. We detect a prominent cyclic
behavior of filament length, PIL length, and coronal hole area with significant
correspondence with the solar magnetic cycle. The spatio-temporal evolution of
the geometric centers of filaments shows a butterfly-like structure and
distinguishable pole-ward migration of long filaments during cycle maxima. We
identify this rush to the poles of filaments to be co-temporal with the
initiation of polar field reversal as gleaned from Mount Wilson and Wilcox
Solar Observatory polar field observations and quantitatively establish their
temporal correspondence. We analyze the filament tilt angle distribution to
constrain their possible origins. Majority of the filaments exhibit negative
and positive tilt angles in the northern and the southern hemispheres,
respectively -- strongly suggesting that their formation is governed by the
overall large-scale magnetic field distribution on the solar photosphere and
not by the small-scale intra-active region magnetic field configurations. We
also investigate the hemispheric asymmetry in filaments, PILs, and coronal
holes. We find that the hemispheric asymmetry in filaments and PILs are
positively correlated -- whereas coronal hole asymmetry is uncorrelated -- with
sunspot area asymmetry.
