1. What have the authors contributed in "Exploring the optical transient sky with the palomar transient factory" ?
In this article the authors present the scientific motivation for PTF and describe in detail the goals and expectations for this experiment.
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2. What are the future works in "Exploring the optical transient sky with the palomar transient factory" ?
The Weizmann Institute PTF partnership is supported by an ISF equipment grant to A. G., whose activity is further supported by a Marie Curie IRG grant from the EU, and by the Minerva Foundation, the Benoziyo Center for Astrophysics, a research grant from Peter and Patricia Gruber Awards, and the William Z. and Eda Bess Novick New Scientists Fund at the Weizmann Institute.
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3. What is the key to a successful transient survey?
The key to a successful transient survey lies in the availability of follow-up resources, specifically multicolor imaging and spectroscopy.
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4. What filters can be used at the telescope?
Observations will be performed mainly in one of two broad-band filters (Mould-R, sdss-g), but additional narrow-band filters (Hα, Hαoff ) can be employed at the telescope.
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![FIG. 1.—R-band peak magnitude as a function of characteristic decay timescale (typically the time to fade from peak by 2 magnitudes) for luminous optical transients and variables. Filled boxes mark well-studied classes with a large number of known members (classical novae, Type Ia supernovae [SNe Ia], core-collapse supernovae [CCSNe], luminous blue variables [LBVs]). Vertically hatched boxes show classes for which only few (≲4) candidate members have been suggested so far (luminous red novae, tidal disruption flares, luminous supernovae). Horizontally hatched boxes are classes which are believed to exist, but have not yet been detected (orphan afterglows of short and long GRBs). The positions of theoretically predicted events (fallback supernovae, macronovae, .Ia supernovae [.Ia]) are indicated by empty boxes. See text for references related to each science case. The brightest transients (on-axis afterglows of GRBs) and events detectable predominantly in the Milky Way (e.g., dwarf novae) are omitted for clarity (see Table 4 for a more complete list). Regions indicate the general location of each class and are not exclusive. Outline colors of boxes correspond to the mean g r color at peak (blue, g r < 0 mag; green, 0≲ g r ≲ 1 mag; red, g r > 1 mag).](/figures/fig-1-r-band-peak-magnitude-as-a-function-of-characteristic-30s4jyb6.webp)
