Emma Salazar Space Telescope

Emma Salazar Space Telescope
Manufacturer	Javelin Industries
Operator	ASANA
Country of origin	Nouvelle Alexandrie
Application	Wide-field optical and near-infrared astronomy
Bus	Custom Javelin observatory bus
Launch mass	6,900 kg
Dimensions	13.2 m long and 4.8 m wide in launch configuration
Power	4.8 kW (beginning of mission)
Equipment	Wide-Field Survey Instrument High-Contrast Coronagraph
Propulsion	Hydrazine monopropellant station-keeping system
Range	Atos-Micras L2
Endurance	5 years planned; consumables for 10 years
Launch date	1764 AN (planned)
Status	In development
Previous mission	Descrubridor Exoplanet Explorer

The Emma Salazar Space Telescope is a planned New Alexandrian wide-field optical and near-infrared space observatory under development by the Aeronautics and Space Administration of Nouvelle Alexandrie (ASANA). The mission leads Celestiales II, a revival of the agency's Celestiales observatory program, and is scheduled for launch aboard an MSS Constellation from the Delgado Space Flight Center in 1764 AN. The observatory is intended to operate in a halo orbit around the second Atos-Micras Lagrange point, about 1.03 million kilometers beyond Micras as measured from Atos.

The telescope combines a 2.4-meter primary mirror with two instruments. Its Wide-Field Survey Instrument has a 0.281-square-degree field of view and is designed for large imaging and spectroscopic surveys. A separate High-Contrast Coronagraph is intended to test the suppression of starlight for direct observation of large exoplanets and circumstellar disks. ASANA has organized the primary science program around wide-area surveys of galaxies, a repeated survey of transient objects, and a microlensing census of planetary systems toward the galactic bulge.

ASANA approved the mission for development in 1760 AN with an estimated total program value of NAX€7.8 billion, including Natopia's in-kind contribution. The NAX€7.35 billion federal appropriation is separate from the advanced-sciences funding authorized by the Aldurian Economic Diversification and Recovery Act, 1755. Javelin Industries is the prime contractor, while New Alexandrian universities and technical institutes supply instrument, thermal-control, and data-system work. Natopia participates through the Joint Space Research Initiative, but ASANA retains mission command, ownership of the observatory, and responsibility for the science archive.

Background

ASANA established the original Celestiales program in 1706 AN as one of its two early programs for astronomy beyond the Atos system. Celestiales missions observed at infrared, visible, ultraviolet, X-ray, and gamma-ray wavelengths, complementing the compact Guardianes Pequeño satellites. The program included the Seiza Space Telescope, Vanguardia Gamma Ray Observatory, Tímido X-Ray Observatory, Ahuanal Infrared Space Telescope, Cedillo Space Telescope, and Descrubridor Exoplanet Explorer before it ended in 1713 AN.

New Alexandrian observational astronomy developed along a different path after Celestiales. The Array for Cosmic Exploration (ACE), a 210-antenna radio interferometer in Santander, entered operation in 1736 AN and supported more than forty research programs by 1751 AN. The joint New Alexandrian and Natopian Interstellar Research and Communication Array became fully operational in 1746 AN, extending deep-space communication and research coverage through seven satellites. Neither installation replaced the wide-field optical and infrared capability that had ended with Celestiales.

ASANA began a new observatory study in 1758 AN, after the Recession of 1757 had produced a federal budget shortfall. The agency placed the study within the subsequent research-policy shift toward technologies that did not depend on Alexandrium. It required the proposed telescope to use a conventional optical train, chemical station-keeping propulsion, and radiation-hardened semiconductor electronics. ASANA's Inti solar-sail demonstrator flew during the study in 1759 AN and performed the first propellantless orbital maneuver by a New Alexandrian spacecraft, but the telescope remained independent of the experimental propulsion programs.

The initial study compared three designs: a 1.5-meter telescope that could be launched in a high Micras orbit, a 2.4-meter survey observatory for the Atos-Micras L2 region, and a 3.5-meter segmented telescope whose cost exceeded the study ceiling. ASANA selected the 2.4-meter design in 1759 AN. The Department of Research and Development authorized Celestiales II the following year, and the observatory was named for Emma Salazar, the test pilot who became the first New Alexandrian woman in space aboard Amanecer-5 in 1696 AN.

Development

The mission is managed by ASANA's Science Mission Directorate from Punta Santiago. The agency retains systems engineering, scientific requirements, launch certification, and flight operations. Javelin Space Systems, the successor to Minerva Space Systems within Javelin Industries, received the prime contract for the observatory bus, telescope structure, instrument integration, and ground-test program. The design uses a five-meter launch envelope compatible with the Constellation launch vehicle rather than a dedicated new rocket.

Instrument development is divided among several existing institutions. The Royal Alexandrian Semiconductor Corporation supplies radiation-hardened readout circuits and flight processors. The corporation also packages and qualifies the focal-plane assemblies. The Royal University of Parap leads detector characterization and optical calibration, while the Institute for Aerospace and Mechanical Engineering conducts structural and vibration testing. ESB Thermodynamics is responsible for the radiators, heat pipes, and instrument thermal enclosure. The mercury-cadmium-telluride sensor wafers are to be fabricated on Natopian-assisted production lines in Alduria under the Cárdenas Protocol. Mission procurement pays for the flight hardware and does not redirect money assigned to the Protocol or the Aldurian Economic Diversification and Recovery Act.

Natopia's in-kind contribution through the Joint Space Research Initiative is capped at NAX€450 million. Its work package covers detector-process support, two deformable mirrors and their wavefront-control electronics, and independent navigation analysis by the initiative's Deep Space Monitoring Integration Facility in Lindström during the transfer to L2. Natopian scientists receive five percent of the general-investigator allocation and may compete for additional time on the same terms as other teams. The agreement gives neither the Natopian government nor a Natopian contractor authority over mission command, survey selection, or release of the New Alexandrian science archive. The commercial launch contract with the NatAlex Launch Alliance is separate from this scientific contribution.

The development schedule provides for a system design review in 1761 AN, completion of the flight mirror in 1762 AN, observatory integration during 1763 AN, and launch readiness in 1764 AN. The primary mirror is designed as a monolithic lightweighted assembly. Its support structure uses conventional low-expansion alloys and composite panels, avoiding a dependence on experimental Alexandrium structures. ASANA reserved a second Constellation launch window in 1765 AN if instrument qualification or launch-vehicle integration exceeds the primary schedule.

Observatory design

The observatory consists of an optical telescope assembly, an instrument carrier, a service module, a fixed sunshield, and a deployable solar array. Its launch mass is projected at 6,900 kilograms. In launch configuration it measures 13.2 meters long and 4.8 meters across; after deployment, the solar array and high-gain antenna extend its span to 16.4 meters. The spacecraft is designed to provide 4.8 kilowatts at the beginning of the mission and at least 4.1 kilowatts after ten years.

The 2.4-meter primary mirror feeds a three-mirror anastigmat with an effective focal ratio of f/7.9. Fine-guidance sensors in the focal plane and vibration-isolated reaction wheels maintain pointing during exposures. A fixed sunshield keeps the telescope assembly near 265 kelvins, while dedicated radiators cool the infrared detector mosaic to about 90 kelvins. After separation from the transfer stage, propulsive maneuvers use a hydrazine monopropellant system for trajectory corrections, momentum unloading, and station keeping.

The command and data system carries 32 terabits, equivalent to 4 terabytes, of solid-state storage. Science data are transmitted in Ka band through a 1.8-meter steerable high-gain antenna at rates of up to 350 megabits per second. The mission is expected to return between 7 and 11 terabits on a normal observing day. X-band equipment provides lower-rate commanding, ranging, and contingency telemetry. ASANA's Deep Space Monitoring Center in Lausanne provides primary tracking and orbit determination during the transfer. The Interstellar Research and Communication Array will provide supplementary ranging and contingency coverage rather than routine mission control.

Wide-Field Survey Instrument

The Wide-Field Survey Instrument is the observatory's principal science instrument. Its focal plane contains eighteen mercury-cadmium-telluride detector arrays, each with 4,096 by 4,096 pixels, providing about 302 megapixels across a field of view of 0.281 square degrees. The image scale is 0.11 arcseconds per pixel. Eight imaging filters cover wavelengths from 0.48 to 2.30 micrometers, spanning visible light and the near infrared.

Two slitless spectroscopy modes share the focal plane. A low-dispersion prism is intended for repeated observations of supernovae and other transients, while a grism provides higher-dispersion spectra for galaxy redshift measurements. Together they cover wavelengths from 0.75 to 1.93 micrometers. A calibration unit mounted behind the instrument entrance supplies flat-field and wavelength references without turning the observatory away from its survey fields.

The instrument's wide field distinguishes the mission from the earlier Cedillo telescope. The camera is optimized to map large, statistically defined samples rather than to examine one small target at a time. ASANA expects a single five-day sequence to image several square degrees to the survey depth, permitting repeated measurements of weak gravitational lensing and stellar brightness without a mosaic of thousands of separate pointings.

High-Contrast Coronagraph

The High-Contrast Coronagraph is a technology demonstrator attached to the second telescope focal station. It uses shaped masks, two deformable mirrors, a low-order wavefront sensor, and an electron-multiplying charge-coupled detector to suppress light from a target star. Its observing band extends from 0.55 to 0.90 micrometers. The design requirement is to distinguish sources up to one hundred million times fainter than their host star at angular separations of several tenths of an arcsecond.

ASANA does not count the coronagraph toward the observatory's minimum science return. Its purpose is to demonstrate wavefront control, autonomous correction of optical drift, and post-processing methods for a later exoplanet-imaging mission. If the instrument meets its full performance requirement, it will directly image several previously identified giant planets and obtain low-resolution spectra of their atmospheres. Failure of the coronagraph would not affect the Wide-Field Survey Instrument or the three primary surveys.

Launch and orbit

The mission is scheduled to launch from platform EL-39 at the Delgado Space Flight Center, which has historically supported MSS Constellation planetary missions. Launch services are provided by the NatAlex Launch Alliance, the joint venture between Javelin Industries and Dingo Enterprises. An MSS Constellation carries the observatory and a disposable transfer stage to a Micras parking orbit. The reusable launcher releases the stack and begins its return for landing. The transfer stage then performs the L2 injection burn. After separation, the telescope deploys its solar array and antenna and begins a transfer lasting about ninety days.

The destination is a large-amplitude halo orbit around the second Atos-Micras Lagrange point. The point lies approximately 1.03 million kilometers from Micras on the line extending away from Atos, a distance derived from the recorded masses and orbit of the two bodies. The orbit keeps Atos, Micras, and Tarsica on the shielded side of the observatory, permits a stable thermal attitude, and provides an uninterrupted view of more than one third of the sky at any time.

Commissioning is planned to last sixty days after arrival. It includes mirror alignment checks, detector calibration, pointing tests, and a staged activation of the coronagraph. The nominal science mission is five years, with propellant reserves and component redundancy sized for ten. ASANA will conduct station-keeping maneuvers about every three weeks and place the observatory in an Atos-centered disposal orbit at the end of operations.

Science program

The reference observing plan assigns seventy-five percent of the five-year primary mission to three core surveys. The remaining twenty-five percent forms a general-investigator program selected through peer review by ASANA and the Federal Science & Research Council. ASANA will freeze field selection and observing cadence after a survey-definition review in 1762 AN. All three core surveys use the Wide-Field Survey Instrument, and their fields are chosen to avoid scattered light from Atos, Micras, and Tarsica.

The High-Latitude Wide Survey will image about 2,000 square degrees outside the galactic plane. Repeated imaging in four infrared bands, accompanied by slitless spectroscopy, will measure galaxy shapes and redshifts for studies of cosmic expansion, weak gravitational lensing, and the distribution of matter. The survey will also produce a catalog of distant galaxies, galaxy clusters, quasars, and faint objects in the outer Atos system.

The High-Latitude Time-Domain Survey will revisit approximately 18 square degrees at a five-day cadence. Its principal targets are supernovae, tidal-disruption events, variable galactic nuclei, and other transients. Prism spectra obtained near maximum brightness will allow researchers to classify events without waiting for follow-up from another observatory. Alerts are scheduled for public release within eighteen hours so that ACE and other facilities can conduct observations at radio wavelengths.

The Galactic Bulge Microlensing Survey will monitor seven fields totaling about two square degrees during six 72-day seasons. Images taken at intervals of fifteen minutes will record gravitational microlensing events caused by stars and planets passing in front of more distant background stars. ASANA designed the cadence to detect planets with orbital distances ranging from the inner regions of their systems to bodies moving without a host star.

General-investigator time may be used for deep fields, nearby galaxies, stellar populations, small bodies, and coronagraph observations. Proposals are evaluated on scientific merit and technical feasibility. Proprietary access is limited to twelve months for investigator programs; core-survey images, calibrated spectra, catalogs, and transient alerts enter the public archive without a proprietary period.

Ground segment and data archive

The Delgado Control Center will command the launch and early flight before handing the observatory to ASANA Mission Control in New Luthoria City. A science operations center at the Array for Cosmic Exploration Data Center in Santander will plan surveys, calibrate instrument data, and operate the public archive. The center will also cross-match transient alerts with ACE observations and IRCA research data. The arrangement connects optical and infrared observations with ACE's established radio-astronomy program without placing either facility under the other's technical control.

The archive expansion provides 18 petabytes of primary storage and two geographically separated copies at Punta Santiago and the Royal University of Parap. Processing is divided into raw telemetry, calibrated exposures, co-added survey images, extracted spectra, and mission catalogs. Public interfaces will support image cutouts and catalog queries so that researchers do not need to transfer complete survey fields. ASANA estimates that the five-year mission will produce between 9 and 13 petabytes of calibrated data and derived products.

Funding and administration

The lifecycle estimate of NAX€7.8 billion at 1760 AN prices covers design, construction, launch, five years of operations, and reserves. The total includes Natopia's NAX€450 million in-kind contribution, leaving a NAX€7.35 billion New Alexandrian federal share. Of the total program value, NAX€4.65 billion is assigned to the telescope, instruments, and spacecraft; NAX€800 million to launch services, the transfer stage, and Delgado modifications; NAX€550 million to the ground system and archive; NAX€650 million to primary operations; and NAX€1.15 billion to schedule and technical reserves. The estimate excludes a possible five-year mission extension, which would require a later appropriation.

The New Alexandrian share is provided through a dedicated federal budget line administered by the Department of Research and Development and ASANA. The appropriation is not charged to the NAX€8 billion advanced-sciences allocation under the Aldurian Economic Diversification and Recovery Act, which supports the Aldurian Science and Technology Campus and Foundation 1768. Hardware purchased from production capacity created under the Cárdenas Protocol remains charged to mission procurement rather than the Protocol's economic-recovery funding. The Federal Science and Research Council funds investigator grants and archival research separately from spacecraft development.

ASANA chairs a program council composed of the mission director, project scientist, chief engineer, Javelin program manager, and representatives of the principal research institutions. The Joint Space Research Initiative holds one non-voting liaison seat for Natopia. An independent review board reports to the Department of Research and Development at each major design and launch-readiness review.

See also

• Aeronautics and Space Administration of Nouvelle Alexandrie
• Inti (spacecraft)
• Array for Cosmic Exploration
• Interstellar Research and Communication Array
• Science and technology in Nouvelle Alexandrie
• NatAlex Launch Alliance