How large is the crater on Titania that is named after Queen of Denmark in Hamlet?
326 km across
Gertrude (Hamlet)
In William Shakespeare's play "Hamlet", Gertrude is Hamlet's mother and Queen of Denmark.
 Her relationship with Hamlet is somewhat turbulent, since he resents her marrying her husband's brother Claudius after he murdered the King (young Hamlet's father, King Hamlet).
 Gertrude reveals no guilt in her marriage with Claudius after the recent murder of her husband, and Hamlet begins to show signs of jealousy towards Claudius.
 According to Hamlet, she scarcely mourned her husband's death before marrying Claudius.
Gertrude (crater)
Gertrude is the largest known crater on Uranus's moon Titania.
 It is about 326 km across, 1/5 of Titania's diameter.
 It is named after the mother of Hamlet in William Shakespeare's play Hamlet.
 Features on Titania are named after female Shakespearean characters.
Rousillon Rupes
Rousillon Rupes is a scarp ("rupes" is Latin for "cliff") on the surface of the Uranian moon Titania named after "Bertram, count of Rousillon" (an Elisabethan English misspelling for Roussillon) in William Shakespeare's comedy All's Well That Ends Well.
 The 402 km long feature is a normal fault situated near the equator and running perpendicular to it.
 The scarp cuts impact craters, which probably means that it was formed at a relatively late stage of moon's evolution, when the interior of Titania expanded and its ice crust cracked as a result.
 Rousillon Rupes has only few crater superimposed on it, which also implies its relatively young age.
 The scarp was first imaged by Voyager 2 spacecraft in January 1986. Stöfler (crater)
Stöfler is a large lunar impact crater located in the crater-riddled southern highlands, named for Johannes Stöffler.
 It sits to the west of the crater Maurolycus.
 At this location, on Earth, the crater appears oval due to foreshortening, but the crater is nearly circular.
 The distorted crater Fernelius is attached to the northern rim, and Miller and Nasireddin lie to the west.
 Faraday has overlain and damaged the western rim, and this crater in turn has been overlain by several smaller craters. Terby (crater)
Terby is a crater on the northern edge of Hellas Planitia, Mars.
 It is in the Iapygia quadrangle.
The 174 km diameter crater is centered at 28°S, 73°E with an elevation of −5 km.
 It is named after François J. Terby.
 It is the site of an ancient lakebed and has clay deposits.
 Using data from Mars Global Surveyor, Mars Odyssey, Mars Express and Mars Reconnaissance Orbiter missions researchers believe Terby's layers were formed from sediments settling under water.
 Crater counts show this happened during the Noachian period.
 It used to be thought that Terby Crater contained a large delta.
 However, newer observations have led researchers to think of the layered sequence as part of a group of layers that may have extended all the across Hellas.
 There is no valley large enough at the northern rim of Terby to have carried the large amount of sediments necessary to produce the layers.
 Other details in the layers argue against Terby containing a delta.
 Fan deposits are some of the thickest on Mars.
 Hydrated minerals, including Fe/Mg phyllosilicates, have been detected in several layers. Columbus (crater)
Columbus Crater is a crater in the Memnonia quadrangle of Mars, located at 29.8° south latitude and 166.1° west longitude.
 It is 119 km in diameter and was named after Christopher Columbus, Italian explorer (1451–1506).
 The discovery of sulfates and clay minerals in sediments within Columbus Crater are strong evidence that a lake once existed in the crater.
 Research with an orbiting near-infrared spectrometer, which reveals the types of minerals present based on the wavelengths of light they absorb, found evidence of layers of both clay and sulfates in Columbus crater.
 This is exactly what would appear if a large lake had slowly evaporated.
 Moreover, because some layers contained gypsum, a sulfate which forms in relatively fresh water, life could have formed in the crater. Haskin (crater)
Haskin is a lunar impact crater located on the lunar far side near the northern pole.
 The crater is located Southwest of the Hevesy crater and the Plaskett crater; the latter of which is located directly adjacent to the large Rozhdestvenskiy crater.
 The crater was adopted and named after American chemist Larry Haskin by the IAU in 2009. Eberswalde (crater)
Eberswalde, formerly known as Holden NE, is a partially buried impact crater in Margaritifer Terra, Mars.
 Eberswalde Crater lies just to the north of Holden Crater, a large crater that may have been a lake.
 The 65.3-km-diameter crater, centered at 24°S, 33°W, is named after the German town of the same name, in accordance with the International Astronomical Union's rules for planetary nomenclature.
 It was one of the final four proposed landing sites for the Mars rover Mars Science Laboratory mission.
 This extraterrestrial geological feature lies situated within the Margaritifer Sinus quadrangle (MC-19) region of Mars.
 Although not chosen, it was considered a potential landing site for the "Mars 2020" rover, and in the second Mars 2020 Landing Site Workshop it survived the cut and was among the top eight sites still in the running. Hamlet (crater)
Hamlet is the largest crater on the known part of the surface of Uranus' moon Oberon.
 It has diameter of about 206 km and is named after the title character of the play Hamlet, by William Shakespeare.
 The crater has a dark floor and is surrounded by a system of bright rays, which are ice ejecta deposited during the impact event.
 The nature of the dark material on the floor is not known, but it may have erupted from depth.
 The crater was first imaged by the Voyager 2 spacecraft in January 1986. Messina Chasma
Messina Chasma is the largest canyon on the surface of the Uranian moon Titania and is named after a location in William Shakespeare's comedy Much Ado About Nothing.
 The 1492 km long chasma is made of two normal faults running NW–SE, which bound a down-dropped crustal block forming a structure called graben.
 The canyon cuts impact craters, which probably means that it was formed at a relatively late stage of the moon's evolution, when the interior of Titania expanded and its ice crust cracked as a result.
 Messina Chasma has only a few crater superimposed on it, which also implies it is relatively young structure.
 The chasma was first imaged by the Voyager 2 spacecraft in January 1986.