Post on 13-Feb-2021
transcript
Northern Sky Transient Survey
w/ Tomo-e Gozen
諸隈 智貴 (東京大学)
Tomoki Morokuma (Univ. of Tokyo/IoA)
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11
Contents
New Parameter Space: High Cadence Transient Surveys
Northern Sky Transient Survey w/ Tomo-e Gozen
Survey Design / Simulation
Follow-up Scheme
Summary
�2
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11 �3Kasliwal 2011, Cooke (http://www.astro.caltech.edu/~ycao/B&ETalks/B&E_FRBs_Cooke.pdf)
128
100 101 102
−24
−22
−20
−18
−16
−14
−12
−10
−8
−6
Characteristic Timescale [day]
Peak
Lum
inos
ity [M
V]
V838 MonM85 OT
M31 RV
SCP06F6
SN2006gySN2005ap SN2008es
SN2007bi
SN2008S
NGC300OT
SN2008ha
SN2005E
SN2002bj
PTF10iuvPTF09dav
PTF11bijPTF10bhp
PTF10fqs
PTF10acbp
PTF09atuPTF09cnd
PTF09cwlPTF10cwr
Thermonuclear Supernovae
Classical Novae
Luminous Red
Novae
Core−Collapse Supernovae
Luminous Supernovae
.Ia Explosions
Ca−rich Transients
P60−M81OT−071213
P60−M82OT−081119
1038
1039
1040
1041
1042
1043
1044
1045
Peak
Lum
inos
ity [e
rg s−
1 ]
Figure 8.1 Framework of Cosmic Explosions in the Year 2011. Note that until 2005 (Fig-
ure 1.1), we only knew about three classes (denoted by gray bands). Systematic surveys,
serendpitous discoveries and archival searches have yielded multiple, new classes of tran-
sients. Discoveries presented in thesis Chapters 3, 5, 6 and 7 are denoted by ⋆.
(Brown et al. 2011) that undergo such an explosion.
2. Luminous Red Novae: The defining characteristics of the emerging class of luminous
red novae (LRN) are: large amplitude (> 7mag), peak luminosity intermediate be-
tween novae and supernovae (−6 to −14mag), very red colors and long-lived infrared
emission. When the first LRN was discovered (Kulkarni et al. 2007), the similarities
to three Galactic explosions (including V838Mon) suggested a common origin. Since
then, 5 more extragalactic and 1 more Galactic LRN have been discovered. Recent
developments suggest there may be two progenitor channels.
http://www.astro.caltech.edu/~ycao/B&ETalks/B&E_FRBs_Cooke.pdf
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11 �4Kasliwal 2011, Cooke (http://www.astro.caltech.edu/~ycao/B&ETalks/B&E_FRBs_Cooke.pdf)
Transients in the local Universe 383
100 101 102
−24
−22
−20
−18
−16
−14
−12
−10
−8
−6
Characteristic Timescale [day]
Peak L
um
inosity [M
V]
V838 MonM85 OT
M31 RV
SCP06F6
SN2006gySN2005ap SN2008es
SN2007bi
SN2008S
NGC300OT
SN2008ha
SN2005E
SN2002bj
PTF10iuvPTF09dav
PTF11bijPTF10bhp
PTF10fqs
PTF10acbp
PTF09atuPTF09cnd
PTF09cwlPTF10cwr
Thermonuclear Supernovae
Classical Novae
Luminous Red
Novae
Core−Collapse Supernovae
Luminous Supernovae
.Ia Explosions
Ca−rich Transients
P60−M81OT−071213
P60−M82OT−081119
1038
1039
1040
1041
1042
1043
1044
1045
Pe
ak L
um
ino
sity [
erg
s−
1]
Figure 4. Framework of Cosmic Explosions in the Year 2011 (Kasliwal 2011). Note that until 2005 (Fig. 1),we only knew about three classes (denoted by gray bands). In the past six years, systematic searches,serendipitous discoveries and archival searches have uncovered a plethora of novel, rare transients. Discov-eries by the Palomar Transient Factory and P60-FasTING (Kasliwal et al. 2011a) are denoted by ?. Severalnew classes are emerging and the governing physics is being widely debated: luminous red novae (electroncapture induced collapse of rapidly rotating O–Ne–Mg white dwarfs?), luminous supernovae (magnetarsor pair instability explosions?), .Ia explosions (helium detonations in ultra-compact white dwarf binaries),Calcium-rich halo transients (helium deflagrations?).
(advanced LIGO, advanced VIRGO, LCGT, INDIGO) coming online. Detecting gravitationalwaves from neutron star mergers every month is expected to become routine. A basic common-ality between gravitational wave searches and the electromagnetic search described above is thatboth are limited to the local Universe (say, < 200 Mpc). A known challenge will be the poor skylocalizations of the gravitational wave signal and consequent large false positive rate of electro-magnetic candidates (Kulkarni & Kasliwal 2009). Therefore, prior to the ambitious search for anelectromagnetic counterpart to a gravitational wave signal, it would only be prudent to build thiscomplete inventory of transients in the local Universe.
Transients in the local Universe 383
100 101 102
−24
−22
−20
−18
−16
−14
−12
−10
−8
−6
Characteristic Timescale [day]
Peak L
um
inosity [M
V]
V838 MonM85 OT
M31 RV
SCP06F6
SN2006gySN2005ap SN2008es
SN2007bi
SN2008S
NGC300OT
SN2008ha
SN2005E
SN2002bj
PTF10iuvPTF09dav
PTF11bijPTF10bhp
PTF10fqs
PTF10acbp
PTF09atuPTF09cnd
PTF09cwlPTF10cwr
Thermonuclear Supernovae
Classical Novae
Luminous Red
Novae
Core−Collapse Supernovae
Luminous Supernovae
.Ia Explosions
Ca−rich Transients
P60−M81OT−071213
P60−M82OT−081119
1038
1039
1040
1041
1042
1043
1044
1045
Pe
ak L
um
ino
sity [
erg
s−
1]
Figure 4. Framework of Cosmic Explosions in the Year 2011 (Kasliwal 2011). Note that until 2005 (Fig. 1),we only knew about three classes (denoted by gray bands). In the past six years, systematic searches,serendipitous discoveries and archival searches have uncovered a plethora of novel, rare transients. Discov-eries by the Palomar Transient Factory and P60-FasTING (Kasliwal et al. 2011a) are denoted by ?. Severalnew classes are emerging and the governing physics is being widely debated: luminous red novae (electroncapture induced collapse of rapidly rotating O–Ne–Mg white dwarfs?), luminous supernovae (magnetarsor pair instability explosions?), .Ia explosions (helium detonations in ultra-compact white dwarf binaries),Calcium-rich halo transients (helium deflagrations?).
(advanced LIGO, advanced VIRGO, LCGT, INDIGO) coming online. Detecting gravitationalwaves from neutron star mergers every month is expected to become routine. A basic common-ality between gravitational wave searches and the electromagnetic search described above is thatboth are limited to the local Universe (say, < 200 Mpc). A known challenge will be the poor skylocalizations of the gravitational wave signal and consequent large false positive rate of electro-magnetic candidates (Kulkarni & Kasliwal 2009). Therefore, prior to the ambitious search for anelectromagnetic counterpart to a gravitational wave signal, it would only be prudent to build thiscomplete inventory of transients in the local Universe.
Transients in the local Universe 383
100 101 102
−24
−22
−20
−18
−16
−14
−12
−10
−8
−6
Characteristic Timescale [day]
Peak
Lum
inos
ity [M
V]
V838 MonM85 OT
M31 RV
SCP06F6
SN2006gySN2005ap SN2008es
SN2007bi
SN2008S
NGC300OT
SN2008ha
SN2005E
SN2002bj
PTF10iuvPTF09dav
PTF11bijPTF10bhp
PTF10fqs
PTF10acbp
PTF09atuPTF09cnd
PTF09cwlPTF10cwr
Thermonuclear Supernovae
Classical Novae
Luminous Red
Novae
Core−Collapse Supernovae
Luminous Supernovae
.Ia Explosions
Ca−rich Transients
P60−M81OT−071213
P60−M82OT−081119
1038
1039
1040
1041
1042
1043
1044
1045
Peak
Lum
inos
ity [e
rg s−1
]
Figure 4. Framework of Cosmic Explosions in the Year 2011 (Kasliwal 2011). Note that until 2005 (Fig. 1),we only knew about three classes (denoted by gray bands). In the past six years, systematic searches,serendipitous discoveries and archival searches have uncovered a plethora of novel, rare transients. Discov-eries by the Palomar Transient Factory and P60-FasTING (Kasliwal et al. 2011a) are denoted by ?. Severalnew classes are emerging and the governing physics is being widely debated: luminous red novae (electroncapture induced collapse of rapidly rotating O–Ne–Mg white dwarfs?), luminous supernovae (magnetarsor pair instability explosions?), .Ia explosions (helium detonations in ultra-compact white dwarf binaries),Calcium-rich halo transients (helium deflagrations?).
(advanced LIGO, advanced VIRGO, LCGT, INDIGO) coming online. Detecting gravitationalwaves from neutron star mergers every month is expected to become routine. A basic common-ality between gravitational wave searches and the electromagnetic search described above is thatboth are limited to the local Universe (say, < 200 Mpc). A known challenge will be the poor skylocalizations of the gravitational wave signal and consequent large false positive rate of electro-magnetic candidates (Kulkarni & Kasliwal 2009). Therefore, prior to the ambitious search for anelectromagnetic counterpart to a gravitational wave signal, it would only be prudent to build thiscomplete inventory of transients in the local Universe.
Transients in the local Universe 383
100 101 102
−24
−22
−20
−18
−16
−14
−12
−10
−8
−6
Characteristic Timescale [day]
Peak
Lum
inos
ity [M
V]
V838 MonM85 OT
M31 RV
SCP06F6
SN2006gySN2005ap SN2008es
SN2007bi
SN2008S
NGC300OT
SN2008ha
SN2005E
SN2002bj
PTF10iuvPTF09dav
PTF11bijPTF10bhp
PTF10fqs
PTF10acbp
PTF09atuPTF09cnd
PTF09cwlPTF10cwr
Thermonuclear Supernovae
Classical Novae
Luminous Red
Novae
Core−Collapse Supernovae
Luminous Supernovae
.Ia Explosions
Ca−rich Transients
P60−M81OT−071213
P60−M82OT−081119
1038
1039
1040
1041
1042
1043
1044
1045
Peak
Lum
inos
ity [e
rg s−
1 ]
Figure 4. Framework of Cosmic Explosions in the Year 2011 (Kasliwal 2011). Note that until 2005 (Fig. 1),we only knew about three classes (denoted by gray bands). In the past six years, systematic searches,serendipitous discoveries and archival searches have uncovered a plethora of novel, rare transients. Discov-eries by the Palomar Transient Factory and P60-FasTING (Kasliwal et al. 2011a) are denoted by ?. Severalnew classes are emerging and the governing physics is being widely debated: luminous red novae (electroncapture induced collapse of rapidly rotating O–Ne–Mg white dwarfs?), luminous supernovae (magnetarsor pair instability explosions?), .Ia explosions (helium detonations in ultra-compact white dwarf binaries),Calcium-rich halo transients (helium deflagrations?).
(advanced LIGO, advanced VIRGO, LCGT, INDIGO) coming online. Detecting gravitationalwaves from neutron star mergers every month is expected to become routine. A basic common-ality between gravitational wave searches and the electromagnetic search described above is thatboth are limited to the local Universe (say, < 200 Mpc). A known challenge will be the poor skylocalizations of the gravitational wave signal and consequent large false positive rate of electro-magnetic candidates (Kulkarni & Kasliwal 2009). Therefore, prior to the ambitious search for anelectromagnetic counterpart to a gravitational wave signal, it would only be prudent to build thiscomplete inventory of transients in the local Universe.
Transients in the local Universe 383
100 101 102
−24
−22
−20
−18
−16
−14
−12
−10
−8
−6
Characteristic Timescale [day]
Peak
Lum
inos
ity [M
V]
V838 MonM85 OT
M31 RV
SCP06F6
SN2006gySN2005ap SN2008es
SN2007bi
SN2008S
NGC300OT
SN2008ha
SN2005E
SN2002bj
PTF10iuvPTF09dav
PTF11bijPTF10bhp
PTF10fqs
PTF10acbp
PTF09atuPTF09cnd
PTF09cwlPTF10cwr
Thermonuclear Supernovae
Classical Novae
Luminous Red
Novae
Core−Collapse Supernovae
Luminous Supernovae
.Ia Explosions
Ca−rich Transients
P60−M81OT−071213
P60−M82OT−081119
1038
1039
1040
1041
1042
1043
1044
1045
Peak
Lum
inos
ity [e
rg s−1
]
Figure 4. Framework of Cosmic Explosions in the Year 2011 (Kasliwal 2011). Note that until 2005 (Fig. 1),we only knew about three classes (denoted by gray bands). In the past six years, systematic searches,serendipitous discoveries and archival searches have uncovered a plethora of novel, rare transients. Discov-eries by the Palomar Transient Factory and P60-FasTING (Kasliwal et al. 2011a) are denoted by ?. Severalnew classes are emerging and the governing physics is being widely debated: luminous red novae (electroncapture induced collapse of rapidly rotating O–Ne–Mg white dwarfs?), luminous supernovae (magnetarsor pair instability explosions?), .Ia explosions (helium detonations in ultra-compact white dwarf binaries),Calcium-rich halo transients (helium deflagrations?).
(advanced LIGO, advanced VIRGO, LCGT, INDIGO) coming online. Detecting gravitationalwaves from neutron star mergers every month is expected to become routine. A basic common-ality between gravitational wave searches and the electromagnetic search described above is thatboth are limited to the local Universe (say, < 200 Mpc). A known challenge will be the poor skylocalizations of the gravitational wave signal and consequent large false positive rate of electro-magnetic candidates (Kulkarni & Kasliwal 2009). Therefore, prior to the ambitious search for anelectromagnetic counterpart to a gravitational wave signal, it would only be prudent to build thiscomplete inventory of transients in the local Universe.
0
log ( [sec])
Transients in the local Universe 383
100 101 102
−24
−22
−20
−18
−16
−14
−12
−10
−8
−6
Characteristic Timescale [day]
Peak
Lum
inos
ity [M
V]
V838 MonM85 OT
M31 RV
SCP06F6
SN2006gySN2005ap SN2008es
SN2007bi
SN2008S
NGC300OT
SN2008ha
SN2005E
SN2002bj
PTF10iuvPTF09dav
PTF11bijPTF10bhp
PTF10fqs
PTF10acbp
PTF09atuPTF09cnd
PTF09cwlPTF10cwr
Thermonuclear Supernovae
Classical Novae
Luminous Red
Novae
Core−Collapse Supernovae
Luminous Supernovae
.Ia Explosions
Ca−rich Transients
P60−M81OT−071213
P60−M82OT−081119
1038
1039
1040
1041
1042
1043
1044
1045
Peak
Lum
inos
ity [e
rg s−1
]
Figure 4. Framework of Cosmic Explosions in the Year 2011 (Kasliwal 2011). Note that until 2005 (Fig. 1),we only knew about three classes (denoted by gray bands). In the past six years, systematic searches,serendipitous discoveries and archival searches have uncovered a plethora of novel, rare transients. Discov-eries by the Palomar Transient Factory and P60-FasTING (Kasliwal et al. 2011a) are denoted by ?. Severalnew classes are emerging and the governing physics is being widely debated: luminous red novae (electroncapture induced collapse of rapidly rotating O–Ne–Mg white dwarfs?), luminous supernovae (magnetarsor pair instability explosions?), .Ia explosions (helium detonations in ultra-compact white dwarf binaries),Calcium-rich halo transients (helium deflagrations?).
(advanced LIGO, advanced VIRGO, LCGT, INDIGO) coming online. Detecting gravitationalwaves from neutron star mergers every month is expected to become routine. A basic common-ality between gravitational wave searches and the electromagnetic search described above is thatboth are limited to the local Universe (say, < 200 Mpc). A known challenge will be the poor skylocalizations of the gravitational wave signal and consequent large false positive rate of electro-magnetic candidates (Kulkarni & Kasliwal 2009). Therefore, prior to the ambitious search for anelectromagnetic counterpart to a gravitational wave signal, it would only be prudent to build thiscomplete inventory of transients in the local Universe.
1""""""""""""""""""""""""""2""""""""""""""""""""""""""3""""""""""""""""""""""""""4"""""""""""""""""""""""""5"""""""""""""""""""""""""6""""""""""""""""""""""""7"
Transients in the local Universe 383
100 101 102
−24
−22
−20
−18
−16
−14
−12
−10
−8
−6
Characteristic Timescale [day]
Peak Lum
inosity [M
V]
V838 MonM85 OT
M31 RV
SCP06F6
SN2006gySN2005ap SN2008es
SN2007bi
SN2008S
NGC300OT
SN2008ha
SN2005E
SN2002bj
PTF10iuvPTF09dav
PTF11bijPTF10bhp
PTF10fqs
PTF10acbp
PTF09atuPTF09cnd
PTF09cwlPTF10cwr
Thermonuclear Supernovae
Classical Novae
Luminous Red
Novae
Core−Collapse Supernovae
Luminous Supernovae
.Ia Explosions
Ca−rich Transients
P60−M81OT−071213
P60−M82OT−081119
1038
1039
1040
1041
1042
1043
1044
1045
Pe
ak L
um
ino
sity [e
rg
s−
1]
Figure 4. Framework of Cosmic Explosions in the Year 2011 (Kasliwal 2011). Note that until 2005 (Fig. 1),we only knew about three classes (denoted by gray bands). In the past six years, systematic searches,serendipitous discoveries and archival searches have uncovered a plethora of novel, rare transients. Discov-eries by the Palomar Transient Factory and P60-FasTING (Kasliwal et al. 2011a) are denoted by ?. Severalnew classes are emerging and the governing physics is being widely debated: luminous red novae (electroncapture induced collapse of rapidly rotating O–Ne–Mg white dwarfs?), luminous supernovae (magnetarsor pair instability explosions?), .Ia explosions (helium detonations in ultra-compact white dwarf binaries),Calcium-rich halo transients (helium deflagrations?).
(advanced LIGO, advanced VIRGO, LCGT, INDIGO) coming online. Detecting gravitationalwaves from neutron star mergers every month is expected to become routine. A basic common-ality between gravitational wave searches and the electromagnetic search described above is thatboth are limited to the local Universe (say, < 200 Mpc). A known challenge will be the poor skylocalizations of the gravitational wave signal and consequent large false positive rate of electro-magnetic candidates (Kulkarni & Kasliwal 2009). Therefore, prior to the ambitious search for anelectromagnetic counterpart to a gravitational wave signal, it would only be prudent to build thiscomplete inventory of transients in the local Universe.
2 1 log ( )
-1 -2 -3 -4
100 Mpc
10 Mpc
http://www.astro.caltech.edu/~ycao/B&ETalks/B&E_FRBs_Cooke.pdf
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11 �5
“Moment” of Supernova Explosion
shock breakout
afterbefore
days
hours
Supernova Shock Breakout
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11 �6
supernova
GW counterpart / kilonova
neutrino counterpart
comet, asteroid
meteor
NEO
space debris
moving objects
pulsar
super-flare, M dwarf flare, CV
Ultra-Long GRB
Fast Radio Burst
AGN
X-ray transient, UV transient
Proposed Science Cases@previous workshops
cadence?survey area?survey region?depth?
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11 �7
no filter: effectively g+r bands
1 visit
6 (3) sec exposure: [0.5 sec exposure] x 12 (6)
~18-19 mag
2x3 or 2x2 dithering
~60 deg2 (partially vignetted by ~30%)
cadence: ~2 hours
survey area / 2 hrs: ~7,000 (10,000) deg2, EL>40 (30) deg
2-4 (3-5) times visits per night
~19 mag for daily stacked data
weather factor: usable (half), photometric (30%)
reference: PS1?
10,000 deg2 - 2 hr cadence - 18 mag depth
10,000 deg2 - 1 day cadence - 19 mag depth
Northern Sky Transient Survey w/ Tomo-e Gozen
(): last year
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11 �8
Tomo-e SN Survey KISSinstrument Tomo-e Gozen KWFC
sensor CMOS CCDreadout time ~0 sec 120 sec
period 2018 fall - 2012/4-2015/9 (3.5 yrs)survey area [deg2] 7,000 50-100
cadence 2 hours / 1 day 1 hourexposure time / visit 6 sec 180 sec
depth 18 mag / 19 mag 20-21 magfilter no (~g+r) g
#(SBOs), #(SNe) / yr 5, 1000 O(0.1)-O(1), 100
data storage daily-stacked image SN cutout images
all data saved
reference - TM, Tominaga, Tanaka+2014
Tomo-e Gozen SN Survey vs Kiso Supernova Survey (KISS) w/ KWFC
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11 �9
Tomo-e Gozen SN Survey vs other SN surveys
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11
Requirements for Survey DesignMultiple visits per night: hopefully N(visit)>=3
Small motion: not go far away for the next pointing
To avoid extra time for telescope pointing (14 sec for 9 deg)
Especially for azimuthal direction (dome rotation)
Not too short time intervals from previous visits: ∂t > 1.5 hours
Not avoid Galactic Plane
Avoid less useful(?) regions?: ~10 < |b| < ~20
Limit the number of visits?
special regions even below Dec. limit?
Higher elevation preferred
�10
b=10b=20
https://faun.rc.fas.harvard.edu/eschlafly/2dmap/Schafly+2014
Extinction map
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11 �11
ELmin delta t min Dec_min Dec_max20180707a 40 90 -5 80
20180707b 40 180 -5 80
20180707c 45 90 -5 80
20180707d 50 90 -5 80
20180707e 35 90 -5 80
20180707f 30 90 -5 80
Survey Simulation
2x2 dithering: some gaps on the sky
too much overlaps in 2x3 dithering
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11 �12
2x3 dithering8.8 deg (diameter)
no gap
but large overlap
2x2 dithering
small gap
small overlap
(to be quantified)
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11
Survey Simulation 1
�13
ELmin delta t min Dec_min Dec_max20180707a 40 90 -5 80
20180707b 40 180 -5 80
20180707c 45 90 -5 80
20180707d 50 90 -5 80
20180707e 35 90 -5 80
20180707f 30 90 -5 80
581 visits (~35,000 deg2)
for 10 hours
# of visits
time interval [hrs]
separation [deg]
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11
Survey Simulation 3
�14
ELmin delta t min Dec_min Dec_max20180707a 40 90 -5 80
20180707b 40 180 -5 80
20180707c 45 90 -5 80
20180707d 50 90 -5 80
20180707e 35 90 -5 80
20180707f 30 90 -5 80
581 visits (~35,000 deg2)
for 10 hours
separation [deg]
time interval [hrs]
# of visits
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11
Survey Simulation 5
�15
ELmin delta t min Dec_min Dec_max20180707a 40 90 -5 80
20180707b 40 180 -5 80
20180707c 45 90 -5 80
20180707d 50 90 -5 80
20180707e 35 90 -5 80
20180707f 30 90 -5 80
X: increase small-#-visit fields
581 visits (~35,000 deg2)
for 10 hours
separation [deg]
time interval [hrs]
# of visits
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11 �16
ELmin delta t min Dec_min Dec_max20180707a 40 90 -5 80
20180707b 40 180 -5 80
20180707c 45 90 -5 80
20180707d 50 90 -5 80
20180707e 35 90 -5 80
20180707f 30 90 -5 80
Survey Simulation Comparison581 visits (~35,000 deg2)
for 10 hours
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11
Follow-up Scheme
�17
After discovering SN candidates…
spectroscopic identification
multi-band light curves
KISS: KISS international collaboration + OISTER
# of spectroscopic observations (29 spec-ID+) limited: too faint
TM+2014, Tanaka+2014, TM+2017, Gabanyi+2018, Kokubo+ in prep.
Tomo-e survey: bright enough for OISTER domestic telescopes
SN: discovery ==> follow-up within the same night
Tomo-e SN Survey
KISS (w/ KWFC)
©Sako
Kyoto/Seimei 3.8m
KOOLS-IFU
optical spectroscopy
optical imaging
Northern Sky Transient Survey 木曽シュミットシンポジウム2018 2018/07/10-11
Northern Sky Transient Survey is being planned and started soon (from this fall).
2x2 dithering, 7,000 deg / 2 hours, 18 mag depth
2-4 visits / night
Do these survey parameter match your sciences?
If yes, suggest any (minor) changes or special options to realize your science cases.
(domestic) Quick follow-up observations
Test observations were done based on previous (worse) simulation.
Image subtraction, data management (DB etc.), quick (and low false-positive) discovery machine development works are being done.
plan to consider weather conditions (avoid cloudy region and choose clear sky region)
need to name the survey (after Tomo-e?)
�18
Summary