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AAVSO Alert Notice 629

Nova in Sagittarius – Nova Sagittarii 2018 = PNV J18040967-1803581

11 April 2018

Event: Nova in Sagittarius – N Sgr 2018 = PNV J18040967-1803581

Discovered independently by:
- Tadashi Kojima (Tsumagoi, Gunma-ken, Japan; reported to CBAT by S. Nakano)
- Hideo Nishimura (Kakegawa, Shizuoka-ken, Japan; reported to CBAT by S. Nakano)
- Yuji Nakamura (Kameyama, Mie, Japan; reported to CBAT by M. Soma)

Discovery magnitude:
- Kojima: unfiltered CCD magnitude 11.2 on six 5-s frames using a Canon EOS 6D digital camera + 200-mm-f.l. f/3.2 lens
- Nishimura: unfiltered CCD magnitude 11.2 on five 10-s frames using a Canon EOS 6D digital camera + 200-mm-f.l. f/3.2 lens
- Nakamura: unfiltered CCD magnitude 11.3 using a CCD camera with 135-mm-f.l. f/4.0 telephoto lens

Discovery date:
- Kojima: 2018 April 8.723 UT
- Nishimura: 2018 April 8.728 UT
- Nakamura: 2018 April 8.788 UT

Coordinates (2000.0): R.A. 18 04 09.45  Decl. -18 03 55.8  (from VSX)
 
Spectra: Spectroscopy indicating that PNV J18040967-1803581 is a nova was obtained by H. Akazawa (Funao Astronomical Observatory, Kurashiki, Okayama, Japan) on 2018 April 09.827 UT using a 0.35-m telescope. The spectrum can be viewed at
http://akazawa-hide.sakura.ne.jp/keijiban/PNVJ18040967_20180409SP.png

J. Rupert et al. (ATel #11528) report: "Our spectrum does not appear to resemble that of a Fe II classical nova early in the outburst. However, if the possible progenitor from Pan-STARRS DR1 reported by P. Schmeer on the TOCP [see Note b below] is related to the transient, then the outburst amplitude is about 12 mag and is comparable to some classical novae. However, the low expansion velocities and the numerous sharp absorption lines suggest that this object may be related to the class of luminous red novae such as V4332 Sgr and V838 Mon."

Observing recommendations: Observations of all types (visual, CCD, DSLR, PEP, spectroscopy) and multiple bands as instrumentation permits are strongly encouraged as the nova evolves.

Observations reported to the AAVSO:
2018 Mar. 27.767, <13.2 unfiltered CCD (T. Kojima; via CBET 4506);
30.786, <13 unfiltered CCD (Y. Nakamura; via CBET 4506);
Apr. 7.723, <14 unfiltered CCD (Nishimura; via CBET 4506);
8.927, 11.74 V (V. Agnihotri, Rawatbhata, India; via R. Fidrich to AAVSO Time Sensitive Alerts forum);
8.927, 13.63 B (Agnihotri; via R. Fidrich to AAVSO Time Sensitive Alerts forum);
9.448, 9.5 unfiltered CCD (G. Masi and M. Schwartz, remotely using a 40.6-cm f/3.75 robotic telescope at Tenagra Observatories near Nogales, AZ; via CBET 4506);
9.644, 13.23 B (S. Kiyota; remotely with an iTelescope 0.50-m f/4.5 CDK astrograph at Siding Spring, NSW, Australia; via CBET 4506);
9.644, 11.01 V (Kiyota; via CBET 4506);
9.644, 9.80 Rc (Kiyota; via CBET 4506);
9.644, 8.52 Ic (Kiyota; via CBET 4506);
9.676, 9.7 unfiltered CCD (T. Noguchi, Chiba-ken, Japan; via CBET 4506);
9.7544, 12.99 B +/-0.006 (A. Pearce, Nedlands, W. Australia);
9.7560, 10.83 V +/-0.002 (Pearce);
9.7575, 8.12 I +/-0.001 (Pearce);
9.803, 10.87 V (K. Yoshimoto, Yamaguchi-ken, Japan; remotely with a 0.50-m f/6.8 reflector at Siding Spring; via CBET 4506);
9.803, 9.62 Rc (Yoshimoto; via CBET 4506);
9.803, 8.30 Ic (Yoshimoto; via CBET 4506);
10.1910, <9.1 (C. Adib, Porto Alegre, Brazil);
10.3597, 11.1 (A. Amorim, Florianapolis, Brazil);
10.4194, 11.0 (L. Shotter, Uniontown, PA);
10.75197, 13.004 B +/-0.005 (Pearce);
10.75345, 10.639 V +/-0.002 (Pearce);
10.7653, 11.3 (Pearce);
11.1250, <11.2 (Amorim).

Charts: Charts with a comparison star sequence for N Sgr 2018 may be created using the AAVSO Variable Star Plotter (VSP).

Submit observations: Please submit observations to the AAVSO International Database using the name N SGR 2018. Once a GCVS name is announced in an IAU Circular or CBET, please use that name.

AAVSO Forums: N Sgr 2018 is the topic of the AAVSO Time Sensitive Alerts forum thread
https://www.aavso.org/pnv-j18040967-1803581-possible-nova-112-mag-sagittarius
and the AAVSO Novae forum thread
https://www.aavso.org/pnv-j18040967-1803581-possible-nova-112-mag-sagittarius-0

Notes:
a. Designated PNV J18040967-1803581 when posted to the IAU Central Bureau for Astronomical Telegrams Transient Object Confirmation Page (TOCP). Unless otherwise noted and except for observations reported to the AAVSO, the information in this Alert Notice is taken from IAU CBET 4506.
 
b. P. Schmeer (Saarbruecken-Bischmisheim, Germany) writes that he has identified a Pan-STARRS DR1 source (magnitude r= 21.89) at position end figures 09.449s, 55.85" as the possible progenitor, adding that he found no previous outbursts or eruptions down to V = 16.1 in images taken by the ASAS-SN Sky Patrol from 2015 February through 2018 March 29.605 UT.

c. Position end figures
 - Kojima (2018 April 8.723 UT): 09.67s, 58.1"
 - Nishimura (2018 April 8.728 UT): 09.46s, 57.3"
 - Nakamura (2018 April 8.788 UT): 09.5s, 04' 01"
 - Masi and Schwartz (2018 April 9.448 UT): 09.46s, 55.6"
 - Noguchi (2018 April 9.676 UT): 09.47s, 55.9"
 - Pearce (2018 April 9.756 UT): 09.46s, 55.7"
 - Yoshimoto (2018 April 9.803 UT): 09.46s, 55.9"
 
d. Images
 - Nishimura (2018 Apr. 8.728 UT): http://www.oaa.gr.jp/~oaacs/image/PNVSgr2018N.JPG  
 - Noguchi (2018 April 9.676 UT): http://park8.wakwak.com/~ngc/images/PNVinSgr_20180409.jpg
 - Yoshimoto (2018 April 9.803 UT): http://orange.zero.jp/k-yoshimoto/PNV-J18040967-1803581_20180409.jpg

Congratulations to Tadashi Kojima, to Hideo Nishimura, and to Yuji Nakamura on their latest discoveries!

This AAVSO Alert Notice was compiled by Elizabeth O. Waagen.


AAVSO Alert Notice 627

Nova Canis Majoris 2018 = TCP J07134590-2112330

26 March 2018

Event: Nova in Canis Major – Nova CMa 2018 = TCP J07134590-2112330

Discovered by: Yuji Nakamura (Kameyama, Mie, Japan) (reported to CBAT by M. Soma, National Astronomical Observatory of Japan)

Discovery magnitude: CCD magnitude 12.0, using a 10-cm f/3 reflector

Discovery date: 2018 March 24.496 UT

Coordinates (2000.0): R.A. 07 13 45.84  Decl. -21 12 31.3  (from VSX)

Spectra: Spectroscopy indicating that TCP J07134590-2112330 is a young classical nova was obtained by J. Strader et al. (ATel #11475) with the 4-m Southern Astrophysical Research Telescope at Cerro Pachon, Chile, on 2018 Mar. 25.1 UT.  

Observing recommendations: Observations of all types (visual, CCD, DSLR, PEP, spectroscopy) and multiple bands as instrumentation permits are strongly encouraged as the nova evolves.

Observations reported to the AAVSO:
2018 March 17.511 UT, <15.4 (Y. Nakamura, Kameyama, Mie, Japan; CBET 4499);
23.153, 15.5 V (ASAS-SN Sky Patrol, as reported by Schmeer; contaminated by the light of a 15th-magnitude star 9" away; CBET 4499);
24.83056, 12.8 (P. Schmeer, Saarbruecken-Bischmisheim, Germany);
25.09593, 12.116 V +/-0.038 (B. Harris, New Smyrna Beach, FL);
25.09677, 13.099 B +/-0.021 (Harris);
25.143, 12.2 V (ASAS-SN Sky Patrol, as reported by Schmeer; CBET 4499);
25.411, 12.14 V (S. Kiyota, Kamagaya, Japan; CBET 4499);
25.411, 11.54 Rc (Kiyota; CBET 4499);
25.411, 11.01 Ic (Kiyota; CBET 4499);
26.04027, 10.820 I +/-0.013 (B. Vietje, South Ryegate, VT);
26.04076, 11.372 R +/-0.010 (Vietje);
26.04142, 12.735 B +/-0.010 (Vietje);
26.04306, 11.9 (L. Shotter, Uniontown, PA);
26.05426, 11.964 V +/-0.008 (Vietje);
26.15483, 11.8965 V +/-0.0092 (S. Shadick, Saskatoon, SK, Canada);
26.13567, 10.7542 I +/-0.0046 (Shadick);

Charts: Charts with a comparison star sequence for N CMa 2018 may be created using the AAVSO Variable Star Plotter (VSP).

Submit observations: Please submit observations to the AAVSO International Database using the name N CMA 2018. Once a GCVS name is announced in an IAU Circular or CBET, please use that name.

AAVSO Forums: N CMa 2018 is the topic of the AAVSO Time Sensitive Alerts forum thread https://www.aavso.org/tcp-j07134590-2112330-new-transient-120-mag-canis-major and the AAVSO Novae forum thread https://www.aavso.org/nova-cma-2018-tcp-j07134590-2112330

Notes:
a. Designated TCP J07134590-2112330 when posted to the IAU Central Bureau for Astronomical Telegrams Transient Object Confirmation Page (TOCP). Unless otherwise noted and except for observations reported to the AAVSO, the information in this Alert Notice is taken from IAU CBET 4499.
 
b. P. Schmeer (Saarbrücken-Bischmisheim, Germany) writes that no previous outbursts or eruptions were recorded by the ASAS-SN Sky Patrol in Feb. 2012 and since Dec. 2014, and he adds that there is a faint (magnitude g = 21.6) Pan-STARRS1 source with position end figures 45.84s, 31.3".  

c. J. Strader et al. (ATel #11475) report that they believe that the nova is identical to the Pan-STARRS1 object noted by Schmeer (Note b).

d. Position end units
- Y. Nakamura (2018 Mar. 24.496 UT, discovery): 45.9s, 33"

Congratulations to Yuji Nakamura on his latest discovery!

This AAVSO Alert Notice was compiled by Elizabeth O. Waagen.


AAVSO Alert Notice 626

Bright nova in Carina – ASASSN-18fv

21 March 2018

Event: Nova Carinae 2018 = ASASSN-18fv

Discovered by: All Sky Automated Survey for SuperNovae (ASAS-SN)

Discovery magnitude: brighter than magnitude 10 V (image was saturated)

Discovery date: 2018 March 20.32 UT

Coordinates (2000.0): R.A. 10 36 13.71  Decl. -59 35 55.1  (from VSX)

Spectra: Spectroscopy indicating that ASASSN-18fv is a classical nova brightening and in the optically thick (Fe curtain) phase was obtained by P. Luckas (ATel #11460) on 2018 March 21.49 UT with an Alpy600 spectrograph having a resolution of about 540 in the range 3800–7300A and using a Atik414 CCD.

Earlier spectroscopy by J. Strader et al. (ATel #11456) had not ruled out a galactic nova, but it was thought the transient might be a large outburst of a young stellar object.

Observing recommendations: Observations of all types (visual, CCD, DSLR, PEP, spectroscopy) and multiple bands as instrumentation permits are strongly encouraged as the nova evolves.

Observations reported to the AAVSO:
2018 March 15.34 UT, <17.0 V (ASAS-SN; ATel #11454);
20.32, >10 V (brighter than 10 V (saturated); ASAS-SN, discovery; ATel #11454);
21.44380, 6.5 (R. Stubbings, Tetoora Road, VIC, Australia);
21.47, 7.19 B (M. Brown et al., Hutton-Westfold Observatory, Monash University; ATel #11457);
21.47, 6.62 V (M. Brown et al.; ATel #11457);
21.47847, 7.4 (A. Pearce, Nedlands, W. Australia);
21.48819, 7.2 (Pearce);
21.54653, 7.1 (Pearce);
21.634, 5.9: (N. Brown, Two Rocks, W. Australia);

Charts: Charts with a comparison star sequence for ASASSN-18fv may be created using the AAVSO Variable Star Plotter (VSP). It is recommended that observers use the binocular chart option if creating an 'a' or 'b' scale chart because there are so many comp stars in the region. Also, we suggest that observers choose the option not to display other variables.

Sebastian Otero notes that a good binocular chart can be obtained using a 300 arc minutes field of view and limiting magnitude 9.0. He provides a link to such a chart:
https://www.aavso.org/apps/vsp/chart/?fov=297.0&star=ASASSN-18fv&orientation=visual&maglimit=9.0&resolution=150&binoc=on&north=down&east=right&type=chart&special=binoc

Submit observations: Please submit observations to the AAVSO International Database using the name ASASSN-18FV. Once a GCVS name is announced in an IAU Circular or CBET, please use that name.

AAVSO Forums: ASASSN-18fv is the topic of the AAVSO Time Sensitive Alerts forum thread https://www.aavso.org/bright-nova-carina and the AAVSO Novae forum thread https://www.aavso.org/asassn-18fv-probable-nova-10-mag-or-brighter-carina

Notes:
a. Unless otherwise noted and except for observations reported to the AAVSO, the information in this Alert Notice is taken from ATels #11454 (K. Z. Stanek et al.), #11456 (J. Strader et al.), #11457 (M. Brown et al.), and #11460 (P. Luckas).

b. Stanek et al. (ATel #11454) note that no outbursts or variability were seen at this location on earlier ASAS-SN images since coverage of the location began in February 2016.

c. Strader et al. (ATel#11456) report that the nova matches to within 0.1" a star in the Gaia DR1 catalog, which has J2000 position end figures 15.4138s 53.648". This star is also present in VPHAS+ DR2 catalog (Drew et al 2014, MNRAS, 440, 2036), with g~20.1 and r ~ 19.5. Magnitude calculations yield g=7.80, r=7.27, i=7.19, B=8.07, V=7.45 for the nova, and imply that the object has brightened by at least 12.3 mag in g.

Congratulations to the ASAS-SN team on this discovery!

This AAVSO Alert Notice was compiled by Elizabeth O. Waagen.


AAVSO Alert Notice 617

Multiwavelength observations of YZ Cnc, SU UMa, and CR Boo outbursts

5 March 2018

Bob Jacobs (Ph.D. candidate, Radboud University) and Drs. Samaya Nissanke (Radboud University), Jennifer Barnes (Columbia University), and Deanne Coppejans (Northwestern University) have requested AAVSO observers' assistance in monitoring the cataclysmic variables YZ Cnc, SU UMa, and CR Boo. The goal is to build good multicolor light curves of two outbursts of CR Boo and two superoutbursts each of YZ Cnc and SU UMa.

Nightly observations of these stars in any Johnson-Cousins band are requested. When an appropriate outburst occurs, observers should switch to multiple observations per night in 3 or more (more preferred) Johnson-Cousins bands (U, B, V, R, I, J, H, K) spread across the spectrum if possible. It is essential to switch to the higher cadence and multiple bands as soon as possible after the outburst begins. Continue until the star returns to minimum, then resume nightly observations. Visual observations are welcome and are encouraged.

The astronomers want to catch the target outbursts as early as possible. If you see an outburst beginning, please notify the AAVSO immediately via the forum thread for this campaign, and submit your observation(s) as soon as possible.

The astronomers provide the following background information: "Last year's Nobel Prize in Physics went to three researchers in the field of gravitational waves. Two weeks later gravitational wave astronomers announced the discovery of a gravitational wave signal from a merger of two neutron stars. This system also emitted optical light right after the merger and it was observed by many telescopes on the southern hemisphere. The new type of transient was called a "kilonova" or "macronova". When two neutron stars merge, they emit large amounts of matter in ejecta (on the order of 1/100th-1/10th the mass of the Sun). These ejecta are neutron rich. Atoms in the ejecta will capture these neutrons and become much heavier than the atoms created in supernovae. They subsequently decay to stable elements like gold and platinum, heating up the ejecta and making it emit optical and infrared light. Kilonovae could account for all of the gold and platinum in the universe. That's why we would like to observe more kilonovae and test this hypothesis (plus many more). Kilonova observations will also put tighter constraints on gravitational waveforms and therefore the theory of General Relativity. Because kilonovae last for only ~10 days, it's important to catch them as early as possible, which requires good observing strategies.

"In order to observe more kilonovae the Radboud University, KU Leuven and NOVA are building the optical telescope BlackGEM in Chile. Upon an alert from the gravitational wave observatories, BlackGEM, together with other observatories, will try to discover the kilonova as quickly as possible. In order to find optimal observing strategies to find the kilonova as quickly as possible, we are trying to simulate how many transients of each type (e.g. Supernovae, dwarf novae, AM CVNs etc.) one would see in what parts of the sky with BlackGEM in each of its color-bands. These transients could be false-positives in the search for the kilonova: they may be indistinguishable from kilonovae. We want to have as few false-positives and as many correctly identified kilonovae as possible. The simulator will also be applicable in other fields of astronomy where estimates are needed for the variability of the night sky.

"For our simulation we use photometry from telescopes to model the temporal evolution of transients. Thanks to the AAVSO community we already have excellent multi-color light curves for SS Cyg and Z Cam type cataclysmic variable outbursts (U Gem and RX And). Unfortunately there aren't yet any light curves available for SU UMa or AM CVn type outbursts with sufficient multi-color coverage to use in our models.

"With your help we look forward to seeing the first well-sampled multi-color observations of CR Boo, SU UMa, and YZ Cnc in outburst."

Coordinates

Name R.A. (2000.0) Dec (2000.0)
YZ Cnc 08 10 56.65 +28 08 33.2
SU UMa 08 12 28.28 +62 36 22.3
CR Boo 13 48 55.22 +07 57 35.7

Charts with comparison star sequences for YZ Cnc, SU UMa, and CR Boo may be plotted using the AAVSO Variable Star Plotter (VSP).

Please submit observations to the AAVSO International Database using the names YZ CNC, SU UMA, and CR BOO.

This observing campaign is being followed on the AAVSO Campaigns and Observing Reports online forum at https://www.aavso.org/yz-cnc-su-uma-cr-boo-outburst-observations

This AAVSO Alert Notice was compiled by Elizabeth O. Waagen.



It’s all about the  standstills, those episodes where the star gets stuck at a mid-point between maximum and minimum. If it doesn’t exhibit standstills it isn’t a Z Cam star.








Data from Catalina Real Time Survey 

Drake et al. 2009, ApJ, 696, 87




Northern CVs brighter than 17th magnitude here.

Southern CV's brighter than 17th magnitude here.



ACTIVITY AT A GLANCE

Last updated 14:46 UT on 19 April 2018

New outbursts and unusual activity reported in the last 72 hours

YYYYMMDD

20180419
WZ CMa
V342 Cen
BP CrA
TU Ind
V699 Oph
V1159 Ori
CL Pup
VZ Pyx
V1830 Sgr

20180418
BF Ara
DM CMa
V436 Car
V803 Cen
EX Dra
IR Gem
VW Hyi (normal outburst)
CRTS J220321.3+144606
DDE 76

20180417
ER UMa
CI UMa
ASASSN-14mr :
ASASSN-15fq
ASASSN-18ik (CV candidate)
MASTER OT J131320.24+692649.1

20180416
CW Mon
NSV 6170
ASASSN-18ij (CV candidate)
CRTS J045959.3-473808


Current superoutbursts (since ...)
AY Lyr : (20180415)
CR Boo (20180413; helium dwarf nova)
RZ LMi (20180413; ER UMa subtype)
1RXS J185310.0+594509 (= DDE 14; 20180412)
YZ Cnc (20180411)
MASTER OT J055845.55+391533.4 (20180406)
V1239 Her (20180403; eclipsing, orbital period 0.100082207 d)
2QZ J112555.7-001639 # (20180401; UGSU, Psh= 0.06481 d; first ever detected outburst)
ASASSN-18gn (20180330; Psh ~0.0745 d)
ASASSN-18go (20180330; Psh= 0.06431 d (stage C))
MASTER OT J181909.82+253407.7 = ASASSN-18ha (20180330, Psh= 0.0585 d)
ASASSN-15me (20180329, superhump period 0.064 ± 0.005 d)
CRTS J072144.4+663838 (20180329, Psh= 0.0819 ± 0.0010 d)
EQ J2143+4612 : (20180329)
HS Vir (20180327)
ASASSN-18gl (20180327; Psh ~ 0.0556 d)
MASTER OT J172758.09+380021.5 #: (20180325; UGSU:)
IR Gem (20180324)
IL Vul (20180323)
RZ LMi (20180322; ER UMa subtype)
NY Ser # (20180322; rebrightening 20180407)
TCP J21290156+3631056 #: (20180322)
ASASSN-18fs # (20180319; UGWZ, Psh= 0.05935 d)
ASASSN-18fk # (20180316; UGWZ, Psh= 0.05944 d (stage B); rebrightenings 20180407 and 0411)


Z Cam-type dwarf novae at standstill
AT Cnc (since 20180202)
TZ Per (since 20171226)
HL CMa (since 20171221) 
IW And (since about 20171219)
NY Ser # (~20180120–20180317, ~56 days; UGSU)
Z Cam (20170405–20171207, 246 days)
IW And (20170812–20170831, 19 days)
OQ Car (20160415–20170826, 498 days)


# indicates a noteworthy or unusual outburst
:  indicates confirmation required
 
'Activity At A Glance' is gleaned from observations reported to AAVSO MyNewsFlash, BAAVSS-Alert, CVnet-Outburst, VSObs-share and VSNET-outburst. We sincerely thank all the observers who contribute timely observations and reports of activity to these email lists.

RECENT PAPERS ON CVs

Updated March 9 2018

For new papers on CV's see arxiv.org astro-ph


Mariko Kimura, Keisuke Isogai, Taichi Kato, Kenta Taguchi, Yasuyuki Wakamatsu, Franz-Josef Hambsch, Berto Monard, Gordon Myers, Shawn Dvorak, Peter Starr, Stephen M. Brincat, Enrique de Miguel, Joseph Ulowetz, Hiroshi Itoh, Geoff Stone, Daisaku Nogami


Joseph Patterson et al.

Paula Szkody, Mark E. Everett, Zhibin Dai, Donald Serna-Grey

John R. Thorstensen, Frederick A. Ringwald, Cynthia J. Taylor, Holly A. Sheets, Christopher S. Peters, Julie N. Skinner, Erek H. Alper, Kathryn E. Weil

Mariko Kato (Keio Univ.), Izumi Hachisu (Univ. of Tokyo), Hideyuki Saio (Tohoku Univ.)

E. Aydi, K. L. Page, N. P. M. Kuin, M. J. Darnley, F. M. Walter, P. Mróz, D. Buckley, S. Mohamed, P. Whitelock, P. Woudt, S. C. Williams, M. Orio, R. E. Williams, A. P. Beardmore, J. P. Osborne, A. Kniazev, V. A. R. M. Ribeiro, A. Udalski, J. Strader, L. Chomiuk


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J.M Hameury & J.P Lasota

V. V. Lukin, K. L. Malanchev, N. I. Shakura, K. A. Postnov, V. M. Chechetkin, V. P. Utrobin



Authors: A. F. Pala, B. T. Gänsicke, D. Townsley, D. Boyd, M. J. Cook, D. De Martino, P. Godon, J. B. Haislip, A. A. Henden, I. Hubeny, K. M. Ivarsen, S. Kafka, C. Knigge, A. P. LaCluyze, K. S. Long, T. R. Marsh, B. Monard, J. P. Moore, G. Myers, P. Nelson, D. Nogami, R. Pickard, G. Poyner, D. E. Reichart, D. Rodriguez Perez, M. R. Schreiber, J. Shears, E. M. Sion, R. Stubbings, P. Szkody, M. Zorotovic


Liam K Hardy, Martin J McAllister, Vik S Dhillon, Stuart P Littlefair, Madelon C P Bours, Elme Breedt, Tim Butterley, Anurak Chakpor, Puji Irawati, Paul Kerry, Tom R Marsh, Steven G Parsons, Chris D J Savoury, Richard W Wilson, Patrick A Woudt
















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