Planets are usually found by observing a star and waiting for the light level to drop when a planet passes in front of it, but what about rogue planets that don't have host stars?
The only way really is through the transit method you describe in your question, however It's pretty much a statistical improbability that a rogue planet will pass through the line of sight between us and another star of which it is not a planetary member.
The Transiting Exoplanet Survey Satellite would provide a glimmer of hope of identifying some of these events. It would require this kind of constant observation since the transit will only occur once and not regularly as an orbiting planet transit would.
A distant stars light could be gravitationally microlensed by the rogue planet, however the planet would have to be very large to produce a noticeable effect (more of a brown dwarf than a rogue planet) and even then the effect would be fleeting.
Direct imaging would be pretty much impossible since the rogue planet would not be close enough to a star to reflect a substantial amount of its light.
Arguably, "rogue planets" have already been discovered by direct imaging.
Giant planets when first formed are big and hot. They radiate their own light, mostly in the infrared. So young isolated planets can be seen directly.
There have been various claims in the literature that objects as small as a few Jupiter masses have been identified in young star forming regions. See various papers by the IAC brown dwarf research group
These claims are open to criticism - sometimes it is hard to tell whether a faint object really belongs to the star forming region observed, rather than being an unassociated background object. The claimed masses also depend heavily on models for the luminosity-mass relation as a function of age, and the ages of these objects are not easily constrained.
Nevertheless it would not be surprising if, in the maelstrom of the formation of a cluster of stars, some planetary systems were stripped from their parent stars by close encounters with other objects.
The chances of seeing older, isolated, planetary mass objects are slim, but microlensing appears to be the only technique presently available. The microlensing signature of a free-floating planet is of course unrepeatable so a discovered planet could not be followed up in any way. However, surveys of microlensing events could be a way of saying something statistically about how common such objects are. See for example http://astrobites.org/2011/05/24/free-floating-planets-might-outnumber-stars/
EDIT: It is also worth noting that the whether these things really are "planets" at all is disputed. They could either be genuine planets, formed in the same way that is hypothesised for most giant planets - that is by accretion onto a rocky core that formed around a star. They could then have been displaced from their parent star by dynamical interactions with other bodies in their system or with a third body. As I said above, N-body simulations do predict that this will happen (e.g. Liu et al. 2013).
On the other hand they could represent the very lowest mass gas fragments that are able to form during the collapse and fragmentation of a molecular cloud and that for some reason were unable to accrete further gas (i.e. they are really more like low-mass brown dwarfs). This so-called "fragmentation limit" is of order 10 Jupiter masses, but if it were a little lower it might explain the free-floating planets that have been seen so far.
Using microlensing the MOA (Microlensing Objects in Astrophysics), OGLE (Optical Gravitational Lensing Experiment) groups have found many free-floating planets.
The stars, free floating planets etc are all moving around the center of our galaxy. They are moving at different speeds, so very occasionally a foreground object passes through the direct line of sight to a background star. When this happens the gravity of the foreground objects acts like a lens magnifying the image of the background star. As the alignment gets better the brightness of the background object appears to brighten. It fades again as the alignment worsens. With very close alignments the apparent brightness of the background star can increase a 1000 fold. The duration of the the rise and fall depends mostly on the mass of the foreground objects. For Jupiter mass planets it's about 4 days, for earth mass planets its on the order of several hours. For a single forground object the rise and fall in brightness of the background star is a very smooth and well known shape. If the foreground object is part of a binary this curve gets distorted with extra bumps, dips and other anomalies.
Note that microlensing does not need to detect any light from the foreground object, so it could be in order of mass, unlit planet free from any star, a very dim star, normal star, white dwarf, neutron star or even a black hole
The MOA and Ogle groups monitor millions of stars per night. They find 1000+ microlensing events per year. A small fraction of these are less than a day in length, and have no signs of extra bumps and wiggles. So they are from free-floating planets.
However measuring the mass of a single lens requires a lot of observations and second order effects. If the background star is large in angular diameter the microlensing light curve it distorted. Modeling these distortions with a estimate of the type of background star, yields and estimate of the mass of the lensing object. If observing the same event from 2 places, it is possible to measure a time delay between when the light arrive at each place. This yields an estimate of the distance to the foreground object. This with knowing the type of the background star yields a mass estimate.
A free-floating planet with a moon has possibly been found. see the MOA web site http://www.phys.canterbury.ac.nz/moa/ for more details about finding rogue planets using microlensing
The Kepler spacecraft and microlensing teams are in a joint campaign, the main aim of which is to detect and then measure the mass of free-floating planet. Because Kepler is far from earth there is a substantial delay between it's light-curves and those measured from earth. See http://www.nasa.gov/feature/ames/kepler/searching-for-far-out-and-wandering-worlds