NRC Herzberg News / Nouvelles du CNRC Herzberg

From/de Dennis Crabtree (NRC-Herzberg)
with contributions from/avec des contributions de Les Saddlemyer & Morrick Vincent

(Cassiopeia – Spring/printemps 2016)

La version française suit

These reports will appear in each issue of Cassiopeia with the goal of informing the Canadian astronomical community on the activities at NRC Herzberg.

Feedback is welcome from community members about how NRC Herzberg is doing in fulfilling our mandate to “operate and administer any astronomical observatories established or maintained by the Government of Canada” (NRC Act).

Integration and Test (I&T) Facility for TMT

The existing integration and test facilities at NRC Herzberg in Victoria were constructed in 1999-2000. In order to maintain Herzberg’s ability to deliver state-of-art instrumentation for TMT, these facilities need to be improved. Specifically, a new I&T facility is required for the construction and testing of NIFIRAOS, the facility adaptive optics system for the TMT.

The new I&T facility will have a 30m by 23m footprint and will be located in an area between an existing parking lot and the side of the sites services building (Figure 1). The new building will be a single story building and consist of three working areas, a Class 1000 Clean Room, a Cold Room, two sets of washrooms, and a Plant Room (Figure 2).

Since the structure is very large, the outside will be finished in a manner to reduce its visibility (Figure 3).

Figure 1.

Figure 1.

Figure 2.

Figure 2.

Figure 3.

Figure 3.

SPIROU Update

SPIROU development is proceeding at a rapid pace. This spring the sub-systems will all come together in Toulouse at the CNRS integration facility. Towards this effort, the staff at the Herzberg Astronomy and Astrophysics labs have been assembling and testing the cryo-mechanical system. This includes the vacuum sub-system, optical mounts and mounting and the precision thermal control system. Final sub-system acceptance testing is scheduled to be complete by the end of May, followed immediately by shipment to Toulouse.

In order to meet the 1 metre/second precision requirement, the optical elements, their mounts and the optical bench must be maintained to a temperature that doesn’t vary by more than +/- 1 milliKelvin over a 24 hour period.

During the past six months, the final fabrication and assembly of the sub-components has been progressing. Examples are the large parabola mount shown in Figure 4 and the 3-prism mount shown in Figure 5.

Figure 4.

Figure 4.

Figure 5.

Figure 5.

Figure 6 shows the SPIROU optical bench mounted on the G10 thermal isolation legs. The radiation shielding and aluminum multi-layer insulation is visible just below. The aluminum frame structure below the shielding supports the entire opto-mechanical structure that will operate at 80K. The full-sized surrogate parabola (~40kg), fold mirror and grating are utilized to provide mass and fitting confirmation without risking the final optical elements at this point in development.

Figure 7 shows the optical bench covered by the active radiation shield. This shield will be actively controlled to a precision of better than 10 milliKelvin in order to have an acceptably small effect on the optical system due to radiation effects.

Figure 6.

Figure 6.

Figure 7.

Figure 7.

With the system almost completely assembled, the next two months will see multiple cool-down cycles to demonstrate reliable operation, tuning of the thermal control system and finalization of the software interfaces.

Figure 8 and Figure 9 show the wrapped thermal critical components being covered up by the moving end of the vacuum vessel for an initial thermal test.

Figure 8.

Figure 8.

Figure 9.

Figure 9.



Les rubriques qui suivent reviendront dans chaque numéro du bulletin et ont pour but de tenir les astronomes canadiens au courant des activités de CNRC Herzberg.

Les commentaires des astronomes sur la manière dont CNRC Herzberg accomplit sa mission, c’est-à-dire « assurer le fonctionnement et la gestion des observatoires astronomiques mis sur pied ou exploités par l’État canadien » (Loi sur le CNRC), sont les bienvenus.

Installation d’intégration et d’essai du Télescope de trente mètres (TMT)

La construction des installations de CNRC Herzberg à Victoria, actuellement utilisées pour l’intégration et les essais des appareils, remonte à 1999-2000. Pour que l’on continue de fournir des instruments à la fine pointe de la technologie au TMT, ces installations devront être rénovées. Plus précisément, on aura besoin d’une nouvelle Installation d’intégration et d’essai pour fabriquer et tester le NIFIRAOS, système d’optique adaptative du TMT.

De 30 m sur 23 m d’envergure, la nouvelle installation sera aménagée à un endroit situé entre le parc de stationnement existant et le côté du bâtiment des services aux sites (figure 1). Il s’agira d’un édifice à un étage regroupant trois aires de travail : une salle blanche de classe 1 000, une salle réfrigérée, deux salles de bain et une salle technique (figure 2).

La structure étant assez imposante, l’extérieur sera aménagé de manière à moins jurer dans le paysage (figure 3).

Figure 1.

Figure 1.

Figure 2.

Figure 2.

Figure 3.

Figure 3.

Le point sur le spectropolarimètre infrarouge (SPIRou)

Le développement du SPIRou va bon train. Ce printemps, les sous-systèmes seront assemblés à Toulouse, à l’installation d’intégration du CNRS. En prévision de cela, le personnel des laboratoires des programmes d’astronomie et d’astrophysique de CNRC Herzberg a monté et testé le système cryomécanique, qui comprend le sous-système sous vide, les fixations des éléments d’optique et les commandes thermiques de précision. Les essais finaux, qui déboucheront sur l’approbation du système, devraient se terminer d’ici la fin du mois de mai et seront immédiatement suivis par l’expédition de l’équipement à Toulouse.

Pour respecter la contrainte d’un mètre/seconde au niveau de la précision, les éléments d’optique, leurs fixations et le banc optique devront être maintenus à une température qui ne variera pas de plus de un millikelvin en 24 heures.

La fabrication et l’assemblage final des sous-éléments ont progressé au cours des six derniers mois, ainsi qu’on peut le constater à la figure 4, illustrant le grand support parabolique, et à la figure 5, représentant la fixation du triple prisme.

Figure 4.

Figure 4.

Figure 5.

Figure 5.

La figure 6 montre le banc optique du SPIRou fixé sur les pattes G10 à isolation thermique. Le bouclier contre les rayonnements et l’isolation faite de nombreuses couches d’aluminium sont visibles immédiatement en dessous. Le cadre en aluminium situé sous le bouclier soutient l’ensemble du système optomécanique, qui fonctionnera à la température de 80 K. Le simulacre de parabole grandeur nature (~40 kg), le miroir de repliement et le réseau permettront d’effectuer les vérifications relatives à la masse et aux ajustements sans que l’on fasse courir de risques aux éléments d’optique finaux à cette étape du développement.

Sur la figure 7, on peut voir le banc optique recouvert du bouclier anti-rayonnement. Celui-ci sera contrôlé dynamiquement à une précision supérieure à dix millikelvins afin que les effets des rayonnements sur le système optique soient assez faibles pour être acceptables.

Figure 6.

Figure 6.

Figure 7.

Figure 7.

Puisque l’assemblage du système est presque chose faite, les deux mois qui suivent verront de nombreux cycles de refroidissement ayant pour buts de prouver la fiabilité opérationnelle du système, d’affiner les réglages des commandes thermiques et de finaliser les interfaces du logiciel.

Les figures 8 et 9 illustrent les composants thermiques essentiels dans leur emballage sur le point d’être couverts par la partie mobile de l’enveloppe sous vide en prévision d’un premier test thermique.

Figure 8.

Figure 8.

Figure 9.

Figure 9.

News from Discover the Universe – Nouvelles d’À la découverte de l’Univers

From/de Julie Bolduc-Duval, coordinator (julie@discovertheuniverse.ca)
(Cassiopeia – Spring/printemps 2016)

La version française suit

As you may know, CASCA has been involved in the teacher-training program Discover the Universe (DU) since its beginning in 2011. Here are some highlights from the last few months:

  • In November 2015, we offered our first international workshop, thanks to funding from the IAU’s Office for Astronomy Development. We reached 176 (French-speaking) teachers from 11 countries on 3 continents. The content of the workshop is now available to astronomy and education professionals in Africa to share with teachers who couldn’t participate in the online workshop due to limited internet access.

    guide activites

  • Funding received in 2015 from the Quebec government allowed us to create an activity kit for afterschool programs. This kit, which includes an 80-page manual as well as 6 videos, is only available in French for now but we would like to translate it in the future. It’s available for free on our website.

  • In 2016, the Dunlap Institute for Astronomy & Astrophysics at the University of Toronto joins us as a major partner. This is great news for us as we are now able to grow our program. Our goal is to develop more resources for teachers and offer more workshops online and across the country. DU remains a national and bilingual program.

If you are interested in teacher training, have already developed resources or simply find the idea interesting, please let me know! We hope to create a network of interested people in different universities and research institutes across Canada.



Comme vous le savez peut-être, CASCA est impliquée dans le programme de formation des enseignants À la découverte de l’Univers (DU) depuis ses tous débuts en 2011. Voici quelques réalisations importantes des derniers mois:

  • En novembre 2015, nous avons offert notre première formation à l’international, grâce à du financement de l’Office for Astronomy Development de l’UAI. Nous avons rejoint 176 enseignants francophones de 11 pays répartis sur 3 continents. Le contenu de la formation est maintenant accessible à des professionnels de l’éducation et de l’astronomie en Afrique afin de la partager avec des enseignants qui ne pouvaient pas participer dans notre formation en ligne dû à un accès internet limité.

    guide activites

  • Grâce à du financement obtenu du gouvernement du Québec sous le programme NovaScience, nous avons développé une trousse d’activités astronomiques pour les groupes parascolaires. Cette trousse, qui inclut un manuel de 80 pages ainsi que 6 vidéos accompagnatrices, est disponible gratuitement sur notre site web. N’hésitez pas à vous y référer si vous voulez des idées d’activités à faire avec les jeunes. La trousse est uniquement disponible en français pour l’instant, mais nous espérons pouvoir la traduire bientôt.

  • En 2016, l’Institut Dunlap pour l’astronomie et l’astrophysique de l’Université de Toronto se joint à nous en tant que partenaire majeur. C’est une excellente nouvelle pour nous, car nous sommes maintenant en mesure de faire croître notre programme. Notre objectif est de développer davantage de ressources pour les enseignants et d’offrir plus d’ateliers en ligne et à travers le pays. DU demeure un programme national et bilingue.

Si vous êtes intéressés par la formation des enseignants du primaire/secondaire, si vous avez déjà développé des ressources ou organisé des évènements pour eux ou si vous êtes simplement intéressés par le sujet, faites-moi signe! Nous espérons créer un réseau de personnes intéressées dans les différentes universités et instituts de recherche partout au pays.

Square Kilometre Array Update

From/de Bryan Gaensler (bgaensler@dunlap.utoronto.ca), Canadian SKA Science Director
(Cassiopeia – Spring/printemps 2016)

For more information on the SKA, subscribe to the Canadian SKA email list and visit the Canadian SKA WWW site.

International SKA Activities

Canada is one of 10 member countries of the SKA Organisation, and is represented on the SKA Board of Directors by Greg Fahlman (NRC) and Bryan Gaensler (University of Toronto). The Board most recently met in July 2015 (Cape Town) and November 2015 (Jodrell Bank). Notable outcomes from these two meetings included:

  • Election of a new Board Chair (Giovanni Bignami, Italy) and Vice-Chair (YIN Jun, China)
  • Discussion of ongoing site characterisation surveys, pre-construction activities, power policies, operations planning, and construction of the SKA headquarters site
  • Approval of a cost-constrained budget for the SKA Organisation for 2016
  • Consideration of a revised schedule and baseline design for SKA1

The next SKA Board meeting will be held on April 4-5, 2016 (Pune).

A SKA Data Flow Advisory Panel (DFAP) has now been convened, with Canada represented by Chris Loken from Compute Ontario. DFAP has been charged with advising the SKA Board on how to optimise the data flow system to ensure that science results can be efficiently extracted. So far, the panel has reviewed analyses of estimated science data production rates, global networking costs, potential archive sizes and the computational requirements for data re-processing and science analysis. The panel has also considered operational, resourcing and governance issues associated with implementing a solution centrally or through regional centres. The panel began its work in the fall of 2015 and held a two day face-to-face meeting in March 2016 to draft a final report.

For further information on international SKA activities, see the latest SKA Newsletter and the monthly SKA Organisation Bulletin.

SKA Intergovernmental Organisation (IGO) Progress

Round 2 of the Treaty Negotiations was held in Rome on January 26-28, 2016. Nine countries were at the negotiating table with formal delegations of typically 3 to 5 people, mainly government officials in ministries responsible for science facilities or the like, with representation from ministries of foreign affairs, or equivalent. Canada was invited as an Observer and Greg Fahlman (General Manager, NRC-HAA) and Gilles Joncas (Chair, ACURA Board of Management) attended.

Good progress was made toward finalising the text of the proposed Treaty Convention that will establish the IGO, but much more work needs to be done in key areas, including the financial arrangements, matters of access to the telescope, procurement and intellectual property rights and policies, as well as the nature of the privileges and immunities required by the project to operate globally. Working groups to deal with these issues were established in the Round 1 session in October 2015 and continue their work between the formal plenary sessions. The working group chairs do share developments with the Canadian Observers although we are not formal participants in the working groups themselves.

The subsequent Round 3 is scheduled for April 19-21, 2016, also in Rome. Canada is again invited as an Observer. This was intended to be the final Round with the convention to be “initialed” and sent back to the respective governments for their internal ratification processes. It is possible that this ambitious goal will not be met and that a subsequent Round will be needed before the key elements of the Treaty are initialed by all Parties. The intent remains to finalise the Convention by the end of 2016 or early 2017. Ratification by five parties, including the three Host countries (UK, Australia, RSA), is required to bring the SKA IGO into existence. This is anticipated to happen by early 2018 in order to initiate procurement activities for the subsequent construction phase.

The principle issues for the Canadian Observers are to ensure scientific access to the facility, with opportunities to influence science priorities and to protect the substantial investment made in developing technology that would be applicable to the SKA. The SKA negotiating parties are aware of Canada’s position and conscious of the need to provide alternatives for countries unable to sign the Treaty to maintain engagement in the Project.

SKA Science and Science Engagement

Development of a new Canadian SKA website has recently been completed, and the site is now live. The site is fully bilingual, and is your starting point for all information about Canadian SKA activities.

The SKA project maintains 11 international science working groups and another 2 focus groups. Membership of science working groups and focus groups is open to all qualified astronomers. If you are interested in joining one of these groups, please contact Bryan Gaensler (bgaensler@dunlap.utoronto.ca).

The Murchison Widefield Array (MWA) is one of three designated SKA precursors (i.e., SKA pathfinders on an SKA site), and is the only one of these three currently operational. Australian government funding has now been awarded for MWA phase 2, which will improve the sensitivity of the array by an order of magnitude. The MWA consortium held its annual project meeting and Board meeting in Toronto over Dec 7-9, 2015. The MWA Board decided to admit a Canadian consortium to the MWA project, led by the University of Toronto; the legal process to add this new Canadian partner is now underway. This will provide Canada with one seat on the MWA Board; Bryan Gaensler has been invited to attend Board meetings as an observer until the admission process is complete.

The first of a roughly annual series of SKA-related science meetings for Canadian astronomers was held in Toronto over December 10-11, 2015 (immediately following the MWA project meeting). This was a very successful meeting, attended by 63 astronomers, ionosphericists and industry representatives from Canada, Australia, India, the USA, New Zealand and the United Kingdom. The meeting featured 25 talks, covering the SKA project, Canadian contributions to SKA science and technology, industry participation, SKA pathfinders, and future Canadian involvement in SKA (see the full program). In the concluding discussion, a plan emerged for a proposal to the CFI Fund, through which we would begin to develop the tools and infrastructure to support a Canadian SKA Data Centre (along with a short-term focus on similar support for VLASS, CHIME and ASKAP). A CFI proposal is now being developed, led by Erik Rosolowsky (Alberta) and Bryan Gaensler (Toronto).

The University of Toronto and the University of Cape Town will jointly host a major conference, “Fundamental Physics with the Square Kilometre Array”, in April 2017 in Mauritius. The goal is to attract the theoretical physics community to the SKA project. Bryan Gaensler (Toronto; chair) and Ingrid Stairs (UBC) are both members of the Scientific Organising Committee for this meeting.

SKA Technology Development

NRC Herzberg continues to be a major participant in pre-construction efforts across several of the SKA design consortia.

NRC has been designated the lead organisation for the Central Signal Processor (CSP) consortium, and is also leading the SKA1-Mid correlator/beamformer. Work is moving forward strongly on the powerMX FPGA platform (code-named Talon), with prototyping activities well underway.

Within the Dish Consortium, the original recommendation proposed for the downselect on the dish structure was to use the NRC rim-supported composite reflectors. However, this recommendation fell short of the 2/3 assent required by the Dish Board, and a new panelised metal reflector design from Germany and China was allowed to compete against the NRC design. A final downselect occurred in November 2015, and the review panel recommended the German/Chinese design over that developed by NRC. This was a surprising decision, and removes NRC from the SKA Dish Structure work. NRC will continue composite reflector research work for higher frequencies, and will support industry interest in commercial reflectors.

NRC continues to lead the Single Pixel Feed digitiser sub-element, passing preliminary design review and preparing to build prototypes in stage 2. The re-baselining addition of Mid band 5 (4.6-13.8 GHz) has added work requiring higher speed samplers to maintain direct conversion. NRC is collaborating with the ALMA high-speed sampler group led by U. Bordeaux, who are developing suitable high-speed samplers. NRC is continuing work on cryogenic low-noise amplifiers for single pixel feeds bands 1 and 2, and has delivered samples to Onsala and EMSS SA, respectively. These same amplifiers have been chosen for MeerKAT, and NRC is in full production with industry partner Nanowave Technologies to deliver MeerKAT bands 1 and 2. NRC will develop prototype band 5 LNAs and submit them for competitive consideration.

Work on phased array feeds (PAFs) is continuing, although the re-baselining decision deleted SKA-Survey and the PAFs from SKA1. NRC is in discussion with CSIRO and ASTRON to form a new advance instrumentation program consortium to continue work on PAFs for SKA. NRC’s L-band PAF was recently equipped with the first room temperature CMOS LNAs from U. Calgary and achieved a hot/cold test system temperature of 20 K. A full prototype to be tested on DVA-1 is being developed. NRC continues to work on cryogenic PAFs, and has moved its concept design to band 4 (2.8-5.2 GHz). A prototype will be produced, again for testing on DVA1.

Within the Telescope Manager (TM) Consortium, NRC is playing a supporting role to NCRA India to develop standards for the local monitor & control software architecture. A standard based on Tango has been developed, and is being ratified for use by all the other consortia.

The SKA’s Science Data Processor (SDP) team is designing the flow of data from the SKA correlator to individual astronomers. A group of Canadian universities and the CADC are working on the SDP design and implementation. The SDP underwent a design review at the beginning of 2015 and the requirements for the SDP are becoming concrete. Regional data centres will be used for the SKA, and discussions are beginning on the path toward establishing a Canadian (North American?) SKA data centre.

ACURA Advisory Council on the SKA

The Association of Canadian Universities for Research in Astronomy (ACURA) coordinates activities and discussion on the SKA through the ACURA Advisory Council on the SKA (AACS). Four new members have been appointed to ACURA for 2016: Gregory Sivakoff (University of Alberta), Samar Safi-Harb (University of Manitoba), Dexter Jagula (SkyWatch) and David Stevens (MacDonald, Dettwiler and Associates). ACURA thanks outgoing AACS members Jeroen Stil, Norbert Bartel, Brian Fry and Don Aldridge for their contributions. A listing of all members of AACS is available.

AACS meets several times per year, with its next meeting on April 21, 2016. For further information or to propose AACS agenda items, please contact the AACS Chair, Bryan Gaensler (bgaensler@dunlap.utoronto.ca).

ALMA Matters

From/de Gerald Schieven
(Cassiopeia – Spring/printemps 2016)

Cycle 4 Call for Proposals

On March 22, the JAO will issue a call for ALMA proposals for Cycle 4, with observations starting 4 October 2016 and running through to the end of September 2017. The proposal deadline is 21 April. Several new capabilities are being offered in Cycle 4, including mm-wave VLBI, solar observing, stand-alone Atacama Compact Array (ACA) proposals, and long-term proposals (>50h). Check the Proposer’s Guide available from the ALMA Science Portal for the full list of capabilities and details about proposing.

Those who would like an in-depth introduction to proposing with ALMA may wish to attend one of the workshops being held March 31 at McMaster University and April 8 at DAO in Victoria. See the next item for more information.

ALMA Days Workshops

The Millimetre Astronomy Group (MAG) at NRC, in their capacity as members of the NAASC supporting ALMA users in North America, will host two “ALMA Days” prior to the Cycle 4 ALMA proposal deadline (21 April 2016). These follow a very successful NRAO Live! event at McGill University in Montreal run by NRAO’s NAASC members with assistance from Brenda Matthews from the MAG. In the coming weeks, members of the MAG will provide 1-day workshops at McMaster University in Hamilton, ON (31 March) and at DAO in Victoria, BC (8 April) to assist those planning ALMA proposals. The focus will be on presenting the ALMA facility, new capabilities and changes to previous modes for Cycle 4, the Observing Tool and using ALMA simulators.

Participants should bring a laptop with the ALMA OT (and CASA — the ALMA DR software — if they wish to test the simulator) installed.

Topics to be covered include:

  • ALMA Overview + Cycle 4 Capabilities
  • Basics of Radio Interferometry
  • The Proposal Process and the Path of ALMA Observations
  • Overview of the ALMA OT
  • Hands-on Session with the OT for proposal preparation
  • The ALMA Simulator Tool in CASA

Those interested in attending should communicate with Brenda Matthews (brenda.matthews@nrc-cnrc.gc.ca).

Forum on Canadian Future of Ground-Based Submm Astronomy, Friday June 3 in Winnipeg

ALMA is now approaching full operations and many members of our Canadian community have applied to and used this facility to further their research goals. At the same time, several groups in Canada are actively involved in ALMA Development opportunities to further the scientific capabilities of this ground-breaking facility (see two reports below). Our community faces a less certain future regarding access to single dish facilities, however. There continues to be uncertainty around CCAT’s schedule and funding status. These difficulties are having an impact on CCAT’s design (such as removing the enclosure) that may affect the potential science of this planned facility. Many researchers in the Canadian community continue to work to maintain Canada’s status in the CCAT project. At the same time, our access to the EAO-operated JCMT has an indeterminate future beyond Jan 31 2017. Access to PI time on the JCMT is open for now to all members of the Canadian community, and many members of the community are involved in the new wave of large surveys with the JCMT. The amount of PI time however is limited. NRC is no longer involved in the management of the JCMT on behalf of the Canadian community, but those actively utilizing JCMT for their science are exploring avenues to provide new instrumentation to the facility.

Given the recommendation of the MTR panel, specifically: “Recommendation: The MTRP reaffirms the importance of next generation single-dish sub-mm facilities, and recommends that Canadian astronomers continue to pursue participation in CCAT, subject to the project meeting its original science goals”, the timing is right for the community to have a frank and open discussion about access to CCAT and JCMT, the timelines for each, and the distribution of effort to ALMA and either or both of these single dish facilities.

Interested members of the community are therefore invited to a face-to-face meeting on the “Status and Future of ground-based submillimetre astronomy in Canada” to follow the CASCA AGM on Friday, 3 June 2016. We will hold the meeting in the CASCA meeting venue from 9am to 12:30pm. The agenda is not yet decided, but we will ask for updates on the three facilities and have lots of time for discussion. There is no charge to attend. We do ask those planning to attend to indicate their interest via email to Erik Rosolowsky (rosolowsky@ualberta.ca) by 27 May 2016.

Call for Development Study Proposals

All interested parties within the North American ALMA partnership are invited to submit proposals for “Development Studies of Upgrades for the Atacama Large Millimeter/submillimeter Array (ALMA)”. Proposals are due 2 May, 2016. Full information about this call, and the level of funding available, can be found at the following link:
science.nrao.edu/facilities/alma/alma-development-cycle4/call-for-proposals-study

This Call is to invite proposals to conduct studies of ideas that may be further developed and implemented in a subsequent funding cycle. The primary aims of this Call for Project Proposals are to:

  • encourage the flow of development ideas from the North American ALMA operations community into the ALMA Development Program Plan;
  • support the development of conceptual and detailed designs by the North American ALMA operations community for possible future inclusion in the ALMA Development Program Plan; and
  • support ALMA-relevant, long-term research and development by the North American operations community.

For examples of ALMA Development Projects that began as Development Studies, see the next two items on CARTA and on Band 3 upgrades.

CARTA – An ALMA Data Analysis and Visualization Tool

Through the ALMA Development Program, the University of Alberta and the University of Calgary are collaborating with NRAO to create CARTA — the Cube Analysis and Rendering Tool for Astronomy. CARTA is a visualization project that aims to provide the functionality of the CASA viewer combined with the stability and performance that comes with a modern application. Currently, the CARTA project has developed the core application and is rapidly implementing new features to deliver the tools that radio astronomy users need. The CARTA project will deliver the software to the ALMA project on Sept. 1st where it will become part of the CASA software package. If you would like to participate in the beta testing of CARTA, please contact Erik Rosolowsky (rosolowsky+carta@ualberta.ca) or visit our webpage to download a beta version.

Band 3 Cartridge Upgrades

Over the past few years, the Millimetre Instrumentation Group at NRC Herzberg in Victoria has been developing and testing options for improving the stability of the Band 3 receivers on ALMA. The solution adopted, block heaters for on-demand magnetic field defluxing of the SIS mixers, has been implemented and validated on one cartridge which has now arrived in Chile. Over the next few years, this upgrade should be gradually applied to all Band 3 cartridges as the Front End cryostats cycle through the ALMA laboratory for routine maintenance. This should result in improved power stability with an additional small enhancement in sensitivity.

ALMA Instructional Videos

The NRC MAG has been producing instructional videos for ALMA. The most recent is a short (6 minute) film on using single-dish data to estimate ALMA sensitivity requirements. An earlier video explores what “Largest Angular Structure” and “Maximum Recoverable Scale” mean.

Jim Hesser is awarded the Schneider Medal

From/de Marilyne Lavoie, Media Relations Officer, NRC
(Cassiopeia – Spring/printemps 2016)

Dr. James (Jim) Hesser, an internationally known astronomer and accomplished NRC manager, is the recipient of the 2015 W.G. Schneider Medal. Dr. Hesser exemplifies the criteria set for the award, which recognizes those who have made outstanding contributions to NRC “above and beyond” the expectations of their job duties and who exemplify NRC values.

Dr. Hesser’s career is marked by decades of scientific leadership and public service in global astronomy and astrophysics. After receiving his PhD from Princeton and starting his astronomy career in Chile, Jim joined NRC as a research officer (RO) in 1977. His leadership skills were soon recognized and in 1986 he was appointed Director of the Dominion Astrophysical Observatory (DAO) in Victoria, BC.

Throughout this 36-year tenure at NRC Dr. Hesser oversaw scientific and technology development work that helped Canada advance its global presence in world astronomy. His service in high offices of all major North American professional societies in his field, as well as on the boards of preeminent international observatories, has strengthened the network of global collaborations that characterize NRC’s Herzberg Astronomy and Astrophysics (NRC Herzberg) programs today.

Jim’s impact has also been profound on NRC and on the broad Canadian astronomy community. Dr. Hesser’s research on the chemical evolution of the early universe through the study of star clusters was ground-breaking and helped attract top talent to NRC for many years. His mentoring helped many prominent astronomers develop their professional careers. Through his long-time involvement in the Victoria chapter of the Royal Astronomical Society of Canada (RASC) and the volunteer-based Scientists and Innovators in the Schools, Jim has done much to bring astronomy to the public at large, culminating with his work as Canadian Chair of the International Year of Astronomy in 2009.

Jim retired as DAO Director – the longest serving in the observatory’s history – in 2014, but his service continues. As Strategic Advisor to the General Manager for NRC Herzberg, he continues to mentor students and researchers while strengthening important stakeholder relationships. This relationship building has contributed to the establishment of the not-for-profit “Friends of the DAO Society” dedicated to supporting science outreach activities at the purpose- built visitor centre playfully named the Centre of the Universe (CU). CU is located adjacent to the NRC observatory’s historic Plaskett telescope.

As NRC celebrates its Centennial year just ahead of the Centennial of that pioneering telescope named after DAO’s founding Director John Stanley Plaskett, it is certainly fitting that an astronomer of Jim Hesser’s calibre is the recipient of the Schneider Medal. “John Plaskett put Canada’s observatory on the map,” notes NRC Herzberg GM Greg Fahlman. “Jim’s legacy is helping keep it there.”

TMT Update – March 2016

By/par Ray Carlberg
(Cassiopeia – Spring/printemps 2016)

TMT planned to have first light in 2017, which would have been wonderful. However, like virtually all major observatories (recall HST, JWST, ALMA) TMT has suffered some (completely novel) bumps in the road. We first lost five years with a funding problem when AURA was removed from the project. Since then we put together a new partnership, collected over a billion dollars and made the decision to release it for construction in April 2015.

The following is my assessment of about where we are, which is largely factual but includes my views of some of the risks and issues that the project must face.

On Dec 2, 2015 the Hawaii Supreme Court (HSC) struck down the Conservation District Use Permit from the Hawaii Board of Land and Natural Resources to the University of Hawaii. TMT itself was not directly involved (the parties were the Board of Land and Natural Resources and the University of Hawaii), although the decision terminates TMT site activity in Hawaii. The HSC identified a process error; in that the permit was granted before a contested case procedure was allowed. The full decision also notes that Conservation Districts have a number of considerations for use and Native Hawaiian consultations that were not clearly followed in the permit process. Independent of the legal situation, the statewide opposition is about 25%, with roughly 60% Native Hawaiians opposed. Canadians would expect to build a major science facility where the local population shares in our excitement of science and views the facility as an item of local pride. Even when TMT had a legal permit, political protest was more than sufficient to prevent site access.

We were invited by a wide ranging group of Hawaiians to consider Mauna Kea as a site. What happened to that support? The concerns about over-use of Mauna Kea arose in the 1990’s and led to the defeat of the Keck outrigger telescope project. A response in Hawaii was to create the Master Plan of 2000, which provided a way forward for astronomy, but at the same time laid out a plan to better regulate the mountain. The MP2000 identified a site for a future giant telescope, which has turned into the TMT site. One aspect of MP2000 is that the TMT site was to be the last site to be developed, leading one US astronomy leader to state that “American astronomy has no long term future in Hawaii”, since in the course of time any astronomy program will inevitably want to build larger, more powerful facilities, which cannot be done under the MP2000. Many, including the Governor of the State, see the Master Plan as not achieving its goals, with Mauna Kea continuing to be over-developed for tourism and insufficient access control. TMT has also become a rallying point for a range of environmental and Native Hawaiian issues, united around stopping TMT. Unless there is a resolution of the Hawaiian situation soon, there will be no support in Canada to continue in Hawaii.

What now? TMT has publicly stated that it plans to restart construction in April 2018 or sooner. To allow the partners to have their resources ready requires that there be a site for which the legal and all other aspects of site access are clearly resolved mid-2017. A good thing is that key Canadian deliverables are not significantly site dependent. We are supplying the enclosure, with Canadian work deliverable items being installed above a base ring and foundation which are costs shared across the project. The Mauna Kea enclosure design can withstand ice-storms and hurricanes, which as a by-product ensure that it can withstand massive earthquakes. The enclosure could be built to the current design and installed almost anywhere. The first light AO system does take into account Mauna Kea atmospheric conditions, but much of what makes AO work is software control which can be modified for a new site.

As of March 1, representatives of the TMT partners have started to travel to various countries and sites that might be suitable sites to host TMT. At the moment this is a fairly wide ranging initiative including sites in both the Northern and Southern hemisphere. Wherever TMT is built it will need to have scientific opportunities that do not simply replicate those available through E-ELT or GMT. Moreover, the decade long delay in getting going means that TMT will need to think carefully about instruments beyond the few initial workhorses to develop powerful competitive instruments that address science, likely in a post-JWST world. So, the good news is that we again have a feasible baseline plan and can be excited about scientific and technical engagement in this great project.

Clearly we would never have selected Hawaii as our preferred site if we had known that we would fail. Given the investment in Hawaii and the many people there who have supported TMT, we need to continue to give Hawaii a chance. It is important to emphasize that a number of people, some associated with TMT, many others in Hawaii, are working hard to help Hawaii be a viable TMT site. However, the pace of activity in Hawaii is not encouraging given our schedule needs. The site permit decision took nearly three months to be remanded back from the courts to the BLNR for them to take action on revising their process to one that could be legally acceptable. Typically the legal steps in getting a permit take about a year, after which the court challenges will start. Although there is ongoing discussion in Hawaii, the opponents remain opposed and are generally believed to have gone from essentially no professional legal support, to potentially very effective and seasoned legal representation. Beyond the law, of course people need to welcome TMT sufficiently that construction can proceed unimpeded. There is also the issue of extending the master lease beyond 2033, which would be essential for TMT and of great interest to a number of other observatories. Some in Hawaii would like to see the summit gradually cleared of all observatories. The Governor’s ten point plan to require that 25% of existing telescopes be removed before TMT is operational is a development that some will see as an encouraging first step in that direction. At the moment the situation does not look all that promising. But, it is not over until it is over and the stakes are fairly high for issues well beyond TMT and astronomy. In the end it is an issue for Hawaiians to solve and they will not be rushed. That is why alternative sites are being assessed with action to be taken soon to maintain schedule.

We very much need to bear in mind that ESO has begun construction of the E-ELT. The ESO finance committee recently approved the procurement of the dome and telescope of the E-ELT, so they are now well on the way. Their plan is to have first light in 2027 under a conservative plan with the existing ESO members. If Brazil joins then they anticipate first light in 2024. GMT continues to move forward with its first light 4 mirror plan (sort-of a double LBT) which gathers a lot more light than an 8m and can do interesting AO work. We need a very good site soon.

ALMA Matters

Submitted by Gerald Schieven
(Cassiopeia – Hivers/Winter 2015)

Cycle 4 Proposal Call Pre-announcement

The JAO has issued a “Pre-announcement” for Cycle 4 proposals, the call for which is expected in March with deadline in April 2016. Among the new capabilities expected in Cycle 4 are:

  • at least 40 antennas in the 12m-Array, 10 in the 7-m Array, and 3 antennas in the Total Power array
  • ACA stand-alone proposals
  • 9 configurations with maximum baseline ranging from 155 m (all Bands), to 12.6 km for Bands 3, 4 & 6, 5.3 km for Band 7, and 2.7 km for Bands 8, 9 & 10
  • solar observing
  • millimetre-wave VLBI in collaboration with the Event Horizon Telescope

Cycle 4 Preparation

Shortly after the call is issued, the NRC Herzberg Millimetre Astronomy Group (MAG) will be holding web tutorials on proposing for ALMA. Details will be sent out in advance through the CASCA exploder and Canadian ALMA user email list (see below) for those who would like to participate. In addition, if your institution is interested in holding a local ALMA workshop, please contact gerald(dot)schieven(at)nrc-cnrc.gc.ca to discuss how the MAG can help.

Cycle 3 Canadian Statistics

Of the 1578 unique proposals submitted to ALMA for Cycle 3, 151 had some participation from people at Canadian institutions (36 as PI). Of these, 44 (6 PI) were awarded high priority (A or B) status, comprising 313 hours of the 2133 hours awarded (~15% of the total). In Cycles 1 and 2, projects with Canadian participation were awarded ~16% and ~11% of the total time respectively. Canadian PI projects were awarded ~18 hours in Cycle 3, roughly 2.6% of the North American allocated time. The number of Canadians involved in ALMA proposals is significant, with 55, 74, and 75 individuals as PI or co-I on all ALMA proposals in Cycle 1, 2 and 3 respectively.

As of October 25, there were 218 refereed publications using ALMA data. Of these, 37, or nearly 18% of the total, had authors or co-authors from Canadian institutions.

ALMA Development Studies

North America issued a call for proposals for ALMA development studies which were due in June 2015. A panel of highly qualified members of the astronomical community reviewed the study proposals. Seven Studies from 34 proposers representing ten institutions in the US and Canada fit within the funding envelope and were proposed for North American funding with the consent of the US National Science Foundation. One of the studies, “Digital Correlator and Phased Array Architectures for Upgrading ALMA”, involves participation by DRAO. Other approved proposals include studies to improve calibration in windows contaminated with atmospheric spectral lines, to enhance visualization of large data sets, and to improve the performance of ALMA’s SIS mixers. Funding will commence in 2016. Further details on these projects can be found in the December NRAO e-News.

Canadian ALMA Users’ email list

A new email distribution list has been created (to replace the previous list which was lost due to the cyber incursion at NRC) for Canadian users of ALMA. The moderated list will be used to distribute information of specific interest to the Canadian ALMA community. Please contact gerald(dot)schieven(at)nrc-cnrc.gc.ca to register for the list.

Data Reduction Party

NRAO is hosting a “Data Reduction Party” January 27-29, 2016, in Charlottesville, VA for people who have ALMA data and want to learn how to get the most science out of them. See this site for more details.

ALMA data reduction is very demanding on processing power and disk space. If you need assistance with ALMA data reduction in any capacity, the NRC Herzberg MAG may be able to help. Please contact Brenda Matthews (brenda(dot)matthews(at)nrc-cnrc.gc.ca) for more information.

Launch of Astrosat

On Sept 28, ISRO launched India’s Astrosat observatory into its planned 600 km, 6 degree inclination orbit. The observatory comprises four X-ray telescopes, and two for UV and blue wavelengths. All instruments are co-aligned, and work simultaneously. Canada has a 5% time-share for providing the solar-blind detectors for UVIT – the UltraViolet Imaging Telescopes. The instruments are all operating, and the mission is in a 6-month period of commissioning and automating of operations. Instrument team demonstration-science observations will be released in April 2016, and team observations will continue until proposal-time observing begins in September. A call for the first Canadian proposals will be issued in ~March, and these may request observations from all instruments. CSA are funding an expert to support Canadian proposals and data processing for UVIT.

NGC 2336 - UVIT, NUV channel, res. = 1.2 arcsec.

NGC 2336 – UVIT, NUV channel, res. = 1.2 arcsec.

Astrosat offers a new and unique facility for Canadian research, and its performance appears to be excellent. UVIT in particular offers wide-field imaging in 3 simultaneous wavelength channels, with ~1” resolution, and a suite of filters and gratings. More
information may be found at this site.

The first UVIT observations were made on Dec 1, following a planned interval to allow for full outgassing. The operations efficiency and data handling are being ramped up slowly, as is normal for a complex space observatory, but the spacecraft and instruments are working well, in some cases exceeding specifications.

Submitted by John Hutchings
(Cassiopeia – Hivers/Winter 2015)

BRITE-Constellation News

Submitted by Gregg Wade
(Cassiopeia – Hivers/Winter 2015)

Introduction

BRITE-Constellation (where BRITE stands for BRIght Target Explorer) is a network of five nanosatellites operating in low Earth orbit, designed to explore the properties of the brightest stars in the night sky.

Figure 1 - The mission patch of the BRITE-Constellation mission.

Figure 1 – The mission patch of the BRITE-Constellation mission.

The BRITE mission is supported by three countries — Canada, Austria and Poland — where Canadian funding comes mainly from the Canadian Space Agency (CSA) and the prime contractor is the University of Toronto Institute for Aerospace Studies – Spaceflight Laboratory (UTIAS-SFL). The mission was planned to have 6 BRITE nanosats, a pair from each partner country, but one of the Canadian nanosats did not detach from the third stage of its launch vehicle.

Each BRITE nanosat (mass = 7 kg; dimensions 20 × 20 × 20 cm) has a 3-cm optical telescope feeding a CCD detector. The Constellation was designed to monitor photometrically through blue and red filters the brightness and temperature variations of stars generally brighter than V ~ 4 with precision, cadence and time coverage not possible from the ground. Each BRITE instrument has an enormous field-of-view: 24° square, large enough to encompass the entire constellation of Orion (but at a resolution of only about half an arcminute per pixel). That means BRITE-Constellation can collect data on several dozens of stars simultaneously.

The sample of the apparently brightest stars in the night sky is a sample dominated by the most intrinsically luminous stars in the Galaxy: hot massive stars at all evolutionary stages, and evolved intermediate-mass stars at the very end of their nuclear-burning phases. The main goals of BRITE-Constellation are to (1) measure the frequencies of pulsations (both acoustic and gravity modes) to probe the interiors and ages of stars through asteroseismology; (2) measure the rotational modulation of stars due to star spots carried across their disks; (3) search for exoplanets through transits; and (4) obtain light curves of massive eclipsing binaries. While goal (2) is often associated with cool solar-type stars, spots in the photospheres of luminous stars could be the sources of co-rotating interaction regions in the winds, possibly arising from magnetic subsurface convection in hot, massive stars.

Figure 2 - Hertzsprung-Russell diagram of the stars of brightest  apparent magnitude, V<4.5. These ∼ 600 stars are the primary BRITE targets.

Figure 2 – Hertzsprung-Russell diagram of the stars of brightest apparent magnitude, V<4.5. These ∼ 600 stars are the primary BRITE targets.[/caption] To develop the optimum data processing and reduction strategies, a BRITE Photometry Tiger Team (PHOTT) was assembled. PHOTT explored and compared various pipelines and ways to minimise data artifacts. To extract the maximum scientific value from the reduced BRITE photometry, the BRITE Ground-Based Observation Team (GBOT) organizes ground-based observing campaigns, primarily high-resolution, high-S/N spectroscopy of BRITE targets. A detailed overview of the scientific motivation of the mission, and technical aspects of the system, are provided by Weiss et al. (2015, PASP 126, 573).

Mission Status and Data Releases

Five of the planned six BRITE nanosats are currently operating in low-altitude (600-800 km) orbits. The first pair of BRITE nanosats (from Austria) were launched on 25 Feb 2013, and the Canadian BRITEs were launched in August 2014 aboard a Russian rocket. The sixth satellite currently remains unusable in a higher elliptical orbit due to a malfunction in the release mechanism of the Russian rocket third stage.

A new ground station capability has been developed at UBC and will soon come on-line, permitting greater data downlink capability.

[caption id="attachment_6337" align="alignright" width="300"]Figure 3 - The two Canadian BRITE nanosatellites (named "BRITE-Montreal", blue filter and "BRITE-Toronto", red filter), at UTIAS-SFL prior to shipment in 2014. Figure 3 – The two Canadian BRITE nanosatellites (named “BRITE-Montreal”, blue filter and “BRITE-Toronto”, red filter), at UTIAS-SFL prior to shipment in 2014.

Seven data releases to BRITE Target PIs have occurred so far. The first was a set of science commissioning data, including (1) about 5 months of quasi-continuous observation of 15 stars in Orion. Subsequent releases were 6-month campaigns of fields in (2) Centaurus and Lupus (30 stars), (3) Sagittarius (18 stars), (4) Cygnus (37 stars), and (5) Perseus (31 stars) . (6) Orion was observed again. Most recently, a field (7) in Vela and Puppis was observed (20 stars). Very soon, data from the recently-completed Scorpius, Cygnus-II and Cassiopeia/Cepheus fields will also be released.

The first BRITE science results have been accepted in refereed journals: a paper by Weiss et al. on the pulsating magnetic star alpha Cir. Weiss et al. (A&A, in press) report two-colour BRITE photometry of this roAp star, excluding quadrupolar modes for the main pulsation frequency, and reporting remarkable differences in the rotationally-modulated flux in the blue and red bandpasses.

Additional papers reporting results for hot, pulsating stars and classical Be stars have also recently been submitted for publication.

The first BRITE science conference, “Science with BRITE Constellation: Initial Results” took place during 14 – 18 September 2015 in Gdansk Sobieszewo, Poland. Presentations authorised for public release are available on the conference website.

A workshop related to a large-scale spectropolarimetric survey of BRITE targets was held at the Meudon
Observatory on October 26-30, with 19 participants. The BRITE spectropolarimetric survey is proceeding nominally, with expected completion in March 2016. Magnetic field has been detected in 47 stars so far, and follow-up observations are being acquired or planned for many of them. Two papers have already been published (Shultz et al. 2015, Neiner et al. 2015) and many others are in preparation. A second BRITE spectropolarimetric workshop will be organized from 14-18 November 2016 at the Meudon Observatory near Paris.

Figure 4 - Light curves of the eclipsing binary V Pup, observed as part of the BRITE Vela/Puppis field. Shown here is a 5-day interval of the BRITE-Austria (blue) and BRITE-Toronto (red) observations.

Figure 4 – Light curves of the eclipsing binary V Pup, observed as part of the BRITE Vela/Puppis field. Shown here is a 5-day interval of the BRITE-Austria (blue) and BRITE-Toronto (red) observations.

Mission Management and Contact

Executive decisions about the mission are made by the BEST (BRITE Executive Science Team), consisting of representatives from all three partner nations. The Canadian BEST members are Tony Moffat (BEST Chair, Université de Montréal), Jaymie Matthews (BEST vice-Chair, UBC), Slavek Rucinski (University of Toronto), and Gregg Wade (Royal Military College), with Jason Rowe (Université de Montréal) and Stefan Mochnacki (University of Toronto) serving as non-voting BEST members.

Setting priorities on BRITE targets and science goals was overseen by BEST, with input from the BRITE International Science Advisory Team (BIAST), consisting of 130 astronomers around the globe. Interested in joining BIAST, to participate in data analysis, and receive monthly mission updates? Please contact BEST through Tony Moffat (moffat@astro.umontreal.ca).

Neiner, C.; Buysschaert, B.; Oksala, M.E.; Blazère, A., 2015, “Discovery of two new bright magnetic B stars: i Car and Atlas”, MNRAS 454, 56

Shultz, M.; Rivinius, Th.; Folsom, C. P.; Wade, G. A.; Townsend, R. H. D.; Sikora, J.; Grunhut, J.; Stahl, O.; and the MiMeS Collaboration, “The magnetic field and spectral variability of the He-weak star HR 2949”, 2015, MNRAS 449, 3945

Weiss, W.W.; Rucinski, S.M.; Moffat, A.F.J.; Schwarzenberg-Czerny, A.; Koudelka, O.F.; Grant, C.C.; Zee, R.E.; Kuschnig, R.; Mochnacki, St.; Matthews, J.M.; Orleanski, P.; Pamyatnykh, A.; Pigulski, A.; Alves, J.; Guedel, M.; Handler, G.; Wade, G.A.; Zwintz, K., 2014, “BRITE-Constellation: Nanosatellites for Precision Photometry of Bright Stars”, PASP 126, 573.

Weiss, W.W.; Frohlich, H.-E.; Pigulski, A.; Popowicz, A.; Huber, D.; Kuschnig, R.; Moffat, A.F.J.; Matthews, J.M.;, Saio, H.; Schwarzenberg-Czerny, A.; Grant, C; Koudelka, O.; Lueftinger, T.; Rucinski, S.; Wade, G.A.; Alves, J.; Guedel, M.; Handler, G.; Mochnacki, S.; Orleanski, P.;, Pablo, B.; Pamyatnykh, A.; Ramiaramanantsoa, T; Rowe, J.; Whittaker, G.; Zawistowski, T.; Zoconska, E.; Zwintz, K., 2015, “The roAp star alpha Cir seen by BRITE-Constellation”, A&A, in press.

Herschel-HIFI News

Submitted by Sylvie Beaulieu, Herschel-HIFI Instrument Support Scientist
(Cassiopeia – Hivers/Winter 2015)
Herschel_spacecraft_artist410

Herschel Science Archive (HSA)

The latest Herschel Science Archive (v.7.0) was released on 28 October 2015. In this release, you will find links from individual observations to associated refereed publications. This new feature is accessible from the query result page in the HSA User Interface by selecting the “DETAILS & PUBLICATIONS” button, and then clicking on the tab “Publications”. Footprints for photometric observations (PACS & SPIRE) greatly improve the accuracy of geometrical searches. Remember that Herschel data are 100% in the public domain.

University of Waterloo Group News

Since last August, the group has welcomed a new member, Dr Scott Jones, who is a recent PhD graduate from Western University. Scott is helping with HIFI data processing and analysis.

Please note that the Herschel-HIFI Waterloo group will cease operation by the 31st of March 2016. Although no support will be available from that date via the Waterloo group, we will try to maintain the webpage and keep it as up-to-date as possible.

The implementation of the Herschel Explanatory Legacy Library (HELL) is progressing well. A special one-week documentation retreat was held in October to allow a group of eight HIFI editors to concentrate on editing the HIFI Handbook, and several other documents that will join the HELL documentation repository. Permanent links to the ESA Herschel Project and to the Herschel Explanatory Legacy Library will be available through our webpage.

Herschel Interactive Processing Environment (HIPE)

While HIPE 13.0 is the current release, and HIFI_CAL_22_0 is the latest Calibration Tree, this autumn saw the last Astronomer Acceptance Testing for HIPE, with HIPE 14.0 due to be released to the community in mid-December 2015. HIFI_CAL_24_0 will also be released. We invite you to visit What’s New in HIPE for the changes in this new release and see below. Additional information can be found in the HIFI Instrument and Calibration page

HIFI Calibration

A new calibration tree has been implemented in HIPE 14.0. It contains substantial changes in the sideband ratio tables, as well as a complete intensity calibration uncertainty component model. The corresponding UncertaintyTable products are available in calibration -> Downlink -> Generic and were updated with the following uncertaintyType: HotLoadTemp, ColdLoadTemp, HotLoadCoupling, ColdLoadCoupling, SidebandRatio, OpticalStandingWavesLoads, OpticalStandingWavesDiplexer.

The new calibration tree also provides tables of spur warning channel flags for point and mapping modes. These flags are assigned based on a knowledgebase built out of the spur flags manually identified for spectral scans and populated in the calibration tree in HIPE 13.0.

The sideband ratio updates will imply changes in intensity at all frequencies in bands 1 to 4. No changes are expected in bands 5 to 7.

The identifyLines task was updated with the following: implementation of threading to speed up the task, improvements of the rejection of false detected lines, changes on the Herschel Spectral Line List columns names, implementation of the image band line identification for pointed and mapping observations, fix to the RMS computation, and the implementation of the exportLines task.

Level 2 Pipeline

For DBS Raster maps, the Level 2 spectra are no longer averaged – this was already the case for OTF maps; Introduction of a new calibration output providing a frequency-dependent intensity calibration uncertainty budget; Assignment of spur warning channel flag for all point and mapping modes.

Level 2.5 Pipeline

Changes to the output of the Deconvolution task: the single-sideband spectrum is now contained in a Spectrum1d called “dataset” (it was called “ssb” up to HIPE 13).

HIFI products

Flags are now applied to OFF spectra as well; Generation of a browse image for the reference spectra, when the option useReferenceSpectra is set to true; The FITS header keywords have been revamped in order to provide proper nicknames to the parameters featured in those headers.

Standing Wave removal

New parameter addMedianContinuum: allow the median continuum to be added back into the baseline fit flux [DEFAULT: False].

Baseline removal

New parameter addMedianContinuum: allow the median continuum to be added back into the baseline fit flux but only performs well for basemode=’sub’ and not basemode=’div’ [DEFAULT: False].

Deconvolution

The output deconvolution product ssb is now called dataset (please note that scripts prior to this change will break).

HiClass Export tool

Although this is not an HCSS development, it should be noted that GILDAS/Class now reads the HCSS-generated FITS without needing any prior conversion as it used to be the case using the HiClass task.

Documentation

With this latest release, you have access to the latest documentation updates for both the HIFI Data Reduction Guide, and the HIFI Pipeline Specification Manual. Specifically, you will find a revamp of the chapter “Flags in HIFI data”, section Quality Flags, and a new chapter called “Understanding the uncertainty table information in your data” has been added to the HIFI Data Reduction Guide.

Conferences, workshops and webinars related to Herschel

The University of Waterloo Herschel-HIFI Support Group is committed to assisting you with accessing data through the Herschel Science Archive (HSA) and in using the Herschel Interactive Processing Environment (HIPE) to process your data. Please do not hesitate to contact us. Our webpage has a dedicated page on Data Processing.