text:
July-2001 Jurisprudence
A.M. No. MTJ-99-1188 July 2, 2001 - JOSE E. GURAY v. FABIAN M. BAUTISTA
A.M. No. P-01-1481 July 5, 2001 - RCBC v. NOEL V. QUILANTANG
G.R. No. 135199 July 5, 2001 - CRISOSTOMO MAGAT, ET AL. v. ALBERT M. DELIZO, ET AL.
G.R. No. 141285 July 5, 2001 - CEBU INSTITUTE OF MEDICINE, ET AL. v. CEBU INSTITUTE OF MEDICINE EMPLOYEES' UNION
G.R. No. 141947 July 5, 2001 - ISMAEL V. SANTOS, ET AL. v. COURT OF APPEALS, ET AL.
G.R. No. 144275 July 5, 2001 - NATIONAL HOUSING AUTHORITY, ET AL. v. COURT OF APPEALS, ET AL.
A.M. No. 97-2-53-RTC July 6, 2001 - RE: FERDINAND J. MARCOS
G.R. No. 132318 July 6, 2001 - PEOPLE OF THE PHIL. v. FERNANDO F. MUERONG
G.R. No. 134114 July 6, 2001 - NESTLE PHIL. v. COURT OF APPEALS, ET AL.
G.R. No. 134779 July 6, 2001 - PEOPLE OF THE PHIL. v. HERSON FLORAGUE, ET AL.
G.R. Nos. 137608-09 July 6, 2001 - PEOPLE OF THE PHIL. v. REMEGIO TAGANNA
G.R. No. 143375 July 6, 2001 - RUTH D. BAUTISTA v. COURT OF APPEALS, ET AL.
G.R. Nos. 131856-57 July 9, 2001 - PEOPLE OF THE PHIL. v. WILLIAM MONTINOLA
G.R. Nos. 85494, 85496 & 195071 July 10, 2001 - CHOITHRAM JETHMAL RAMNANI, ET AL. v. COURT OF APPEALS, ET AL.
G.R. No. 126166 July 10, 2001 - PEOPLE OF THE PHIL v. ALLAN TEJADA
G.R. No. 133928 July 10, 2001 - PEOPLE OF THE PHIL. v. NECESARIO HIJAPON, ET AL.
G.R. No. 136267 July 10, 2001 - PEOPLE OF THE PHIL. v. FIDEL ABRENICA CUBCUBIN, JR.
G.R. Nos. 142801-802 July 10, 2001 - BUKLOD NG KAWANING EIIB, ET AL. v. RONALDO B. ZAMORA, ET AL.
A.M. No. MTJ-00-1253 July 11, 2001 - KIAT REAPORT, ET AL. v. EFREN S. MARIANO
A.M. No. P-01-1452 July 11, 2001 - FERMA C. PORTIC v. MARIO B. LOPEZ, ET AL.
G.R. No. P-01-1479 July 11, 2001 - OFFICE OF THE COURT ADMINISTRATOR v. RUBEN B. ALBAYTAR
G.R. No. 104802 July 11, 2001 - AURELIA S. LLANA, ET AL. v. COURT OF APPEALS, ET AL.
G.R. Nos. 108301 & 132539 July 11, 2001 - MANILA ELECTRIC COMPANY v. COURT OF APPEALS, ET AL.
G.R. No. 108346 July 11, 2001 - MARIANO Z. VELARDE, ET AL v. COURT OF APPEALS, ET AL.
G.R. No. 135210 July 11, 2001 - COMMISSIONER OF INTERNAL REVENUE v. ISABELA CULTURAL CORP.
G.R. No. 137050 July 11, 2001 - PEOPLE OF THE PHIL. v. GEORGE CORTES
G.R. No. 137891 July 11, 2001 - PEOPLE OF THE PHIL. v. JESUS PATRIARCA
G.R. No. 140365 July 11, 2001 - CESAR P. UY, ET AL v. VICTORINO P. EVANGELISTA, ET AL.
G.R. No. 140974 July 11, 2001 - RAMON ORO v. GERARDO D. DIAZ
A.M. No. MTJ-01-1349 July 12, 2001 - BERNADETTE MONDEJAR v. MARINO S. BUBAN
G.R. No. 101974 July 12, 2001 - VICTORIA P. CABRAL v. COURT OF APPEALS, ET AL.
G.R. No. 102313 July 12, 2001 - R. F. NAVARRO & CO. v. FORTUNATO A. VAILOCES, ET AL.
G.R. Nos. 102696, 102716, 108257 & 120954 July 12, 2001 - ALBERTO LOOYUKO, ET AL. v. COURT OF APPEALS, ET AL.
G.R. No. 104223 July 12, 2001 - TIBURCIO SAMONTE v. COURT OF APPEALS, ET AL.
G.R. No. 104383 July 12, 2001 - PEOPLE OF THE PHIL. v. VALERIANO AMESTUZO, ET AL.
G.R. No. 112590 July 12, 2001 - STATE INVESTMENT HOUSE v. COURT OF APPEALS, ET AL.
G.R. Nos. 131638-39 July 12, 2001 - PEOPLE OF THE PHIL. v. LORETO D. MEDENILLA
G.R. No. 138737 July 12, 2001 - FINMAN GEN. ASSURANCE CORP., v. COURT OF APPEALS, ET AL.
G.R. No. 138576-77 July 13, 2001 - PEOPLE OF THE PHIL. v. JIMMY JACOB
A.M. No. MTJ-00-1322 July 17, 2001 - RENATO H. SANCHEZ v. GEMINIANO A. EDUARDO
A.M. No. P-01-1484 July 17, 2001 - JOSE R. ASTORGA v. NICOLASITO S. SOLAS
G.R. Nos. 103550 & 103551 July 17, 2001 - PEOPLE OF THE PHIL v. ROMERICO PORRAS
G.R. No. 133814 July 17, 2001 - PEOPLE OF THE PHIL. v. ANDRES ORTIZ
G.R. Nos. 134540-41 July 18, 2001 - PEOPLE OF THE PHIL v. DIONISIO BATALLER
G.R. Nos. 109559 & 109581 July 19, 2001 - BERNARDO P. ABESAMIS, ET AL. v. COURT OF APPEALS, ET AL.
G.R. No. 111535 July 19, 2001 - PEOPLE OF THE PHIL. v. ALEJANDRO CAMPOS
G.R. Nos. 113255-56 July 19, 2001 - PEOPLE OF THE PHIL. v. ROMEO S. GONZALES
G.R. No. 125698 July 19, 2001 - PEOPLE OF THE PHIL. v. FRANCISCO E. HAPA, ET AL.
G.R. Nos. 128153-56 July 19, 2001 - PEOPLE OF THE PHIL. v. VICENTE P. BUISON
G.R. No. 131216 July 19, 2001 - LEONARDO A. QUISUMBING, ET AL. v. COURT OF APPEALS, ET AL.
G.R. No. 132177 July 19, 2001 - JOSE F. CAOIBES v. OMBUDSMAN, ET AL.
G.R. No. 133190 July 19, 2001 - PEOPLE OF THE PHIL. v. SANTOS LOR
G.R. No. 135145 July 19, 2001 - PEOPLE OF THE PHIL. v. RAYMOND G. MAXION
G.R. No. 137545 July 19, 2001 - TERESITA D. GAITE v. COURT OF APPEALS, ET AL.
G.R. No. 139789 July 19, 2001 - POTENCIANO ILUSORIO, ET AL. v. ERLINDA K. ILUSORIO BILDNER, ET AL.
G.R. No. 139967 July 19, 2001 - PEOPLE OF THE PHIL. v. MANUEL TALAVERA
G.R. Nos. 141011 & 141028 July 19, 2001 - CITYTRUST BANKING CORP. v. ISAGANI C. VILLANUEVA
G.R. No. 144179 July 19, 2001 - PEOPLE OF THE PHIL. v. RAMSHAND C. THAMSEY
A.M. No. MTJ-01-1350 July 20, 2001 - LORENZO PASCUAL, ET AL. v. CESAR M. DUMLAO
G.R. No. 110263 July 20, 2001 - ASIAVEST MERCHANT BANKERS (M) BERHAD v. COURT OF APPEALS, ET AL.
G.R. No. 117187 July 20, 2001 - UNION MOTOR CORP. v. COURT OF APPEALS, ET AL.
G.R. No. 120176 July 20, 2001 - MA. VALENTINA SANTANA-CRUZ v. COURT OF APPEALS, ET AL.
G.R. No. 124442 July 20, 2001 - PEOPLE OF THE PHIL. v. ARMANDO S. COMPACION
G.R. No. 132926 July 20, 2001 - ELVIRA AGULLO v. SANDIGANBAYAN, ET AL.
G.R. No. 133580 July 20, 2001 - PEOPLE OF THE PHIL. v. MAXIMO GENEBLAZO
G.R. Nos. 135030-33 July 20, 2001 - PEOPLE OF THE PHIL. v. MERCY LOGAN
G.R. No. 135666 July 20, 2001 - PEOPLE OF THE PHIL. v. MELCHOR B. GARCIA
G.R. No. 135865 July 20, 2001 - NAGKAKAISANG KAPISANAN KAPITBAHAYAN SA COMMONWEALTH AVE. v. COURT OF APPEALS, ET AL.
G.R. No. 138501 July 20, 2001 - PEOPLE OF THE PHIL. v. ERNESTO M. LAXA, ET AL.
G.R. No. 139150 July 20, 2001 - PABLO DELA CRUZ v. COURT OF APPEALS, ET AL.
G.R. No. 142024 July 20, 2001 - GUILLERMO SARABIA v. PEOPLE OF THE PHIL.
G.R. No. 145838 July 20, 2001 - NICASIO I. ALCANTARA v. COMMISSION ON THE SETTLEMENT OF LAND PROBLEMS, ET AL.
G.R. No. 146079 July 20, 2001 - KANEMITSU YAMAOKA v. PESCARICH MANUFACTURING CORP., ET AL.
A.M. No. RTJ-00-1564 July 26, 2001 - MARISSA M. GORDON, ET AL. v. FRISCO T. LILAGAN
G.R. Nos. 132325-26 July 26, 2001 - PEOPLE OF THE PHIL. v. ROMEO ESPINA
G.R. No. 133225 July 26, 2001 - PEOPLE OF THE PHIL. v. EDWIN CONCEPCION, ET AL.
G.R. Nos. 113176 & 113342 July 30, 2001 - HANIL DEVELOPMENT CO. v. COURT OF APPEALS, ET AL.
A.M. Nos. P-00-1381 & A.M. No. P-00-1382 July 31, 2001 - EFREN B. MALLARE v. RONALD ALLAN A. FERRY
G.R. No. 105647 July 31, 2001 - ERNESTO BIONA v. COURT OF APPEALS, ET AL.
G.R. Nos. 121298 & 122123 July 31, 2001 - GENARO RUIZ, SR., ET AL. v. COURT OF APPEALS, ET AL.
G.R. No. 129329 July 31, 2001 - ESTER M. ASUNCION v. NLRC, ET AL.
G.R. No. 130707 July 31, 2001 - VERONICA ROBLE, ET AL. v. DOMINADOR ARBASA, ET AL.
G.R. No. 134634 July 31, 2001 - PEOPLE OF THE PHIL. v. LAZARO CLARIÑO, ET AL.
G.R. Nos. 134831-32 July 31, 2001 - PEOPLE OF THE PHIL. v. RAMON N. LOGMAO
G.R. Nos. 136827 & 136799 July 31, 2001 - SECRETARY OF AGRARIAN REFORM, ET AL. v. TROPICAL HOMES
G.R. No. 136847 July 31, 2001 - PEOPLE OF THE PHIL v. RODULFO P. VILLARIN, ET AL.
G.R. No. 138289 July 31, 2001 - GRACIANO PALELE v. COURT OF APPEALS, ET AL.
G.R. No. 139180 July 31, 2001 - PEOPLE OF THE PHIL. v. ROLANDO RIVERA
G.R. No. 139529 July 31, 2001 - PEOPLE OF THE PHIL. v. TIMOTEO BRACERO
G.R. No. 139622 July 31, 2001 - PEOPLE OF THE PHIL. v. PEDRO PERRERAS, ET AL.
G.R. No. 142616 July 31, 2001 - PHIL. NATIONAL BANK v. RITRATTO GROUP INC., ET AL.
G.R. No. 143687 July 31, 2001 - RAMON ESTANISLAO, ET AL. v. COURT OF APPEALS, ET AL.
G.R. No. 144702 July 31, 2001 - U.I.C. ET AL. v. U.I.C. TEACHING AND NON-TEACHING PERSONNEL AND EMPLOYEES UNION, ET AL.
G.R. No. 145389 July 31, 2001 - ANIANO A. DESIERTO, ET AL. v. RONNIE C. SILVESTRE
Philippine Supreme Court Jurisprudence > Year 2001 > July 2001 Decisions > G.R. Nos. 136827 & 136799 July 31, 2001 - SECRETARY OF AGRARIAN REFORM, ET AL. v. TROPICAL HOMES:
[G.R. No. 136827. July 31, 2001.]
THE SECRETARY OF AGRARIAN REFORM, THE REGIONAL DIRECTOR FOR REGION XI, ALEJO V. DUQUE, MNSA and THE PROVINCIAL AGRARIAN REFORM OFFICER OF DAVAO CITY, JUAN C. BARROT, BOTH OF THE DEPARTMENT OF AGRARIAN REFORM, FARMERS-BENEFICIARIES REYNALDO H. BASALAN, AUREO H. BASALAN, JUSTINA FROILAN, PEDRO T. OROYAN, and THE REST OF THE PRIVATE RESPONDENTS IN DARAB CASE NO. XI-1112-DC-94 (DARAB APPEAL CASE NO. 6047/CA-G.R. SP NO. 46262), Petitioners, v. TROPICAL HOMES, INC., Respondent.
SECRETARY OF AGRARIAN REFORM, REGIONAL DIRECTOR, REGION XI and PROVINCIAL AGRARIAN REFORM OFFICER, DAVAO CITY, BOTH OF THE DEPARTMENT OF AGRARIAN REFORM, TOMASA T. ESTILLORE, FELIX S. GICALA, ERLINDA P. MALACURA, AGUIDO A. BENTAZA, ERNESTO MANIEGO, SANDY M. PADRIGON, BENJAMIN P. CAMINADE, EVELIO P. RICA, VICTORIA P. BISNAR, INOCENTIS CAMUS, RODRIGO B. LUCES, ELIAS C. MANIEGO, PACIFICO H. BASALAN, AMBROSIO L. GEALON, AMADA P. TUBIG, JULIANO A. MASIN, LEONORA S. VILLAMOR, ORCISIA D. ANTANG, AQUILINA M. SORIA, ANASTACIO A. DUMLAO, JIMMY ABAYAN OTIDA, JUANEVE D. PERIQUIT, NUMERIANO C. CAMINADE, WILFREDO A. MARQUEZ, DOMINADOR FANO ANDALES, AGUSTINA G. CARDONA, CESAR J. LABELLA, MAMERTO G. ESPERANZA, NAVALES WALDO B. DELINA, VISITACION TAYO DATOR, NORMA C. PACYAO, EXPEDITA BALDERAMA SELARGA, DOROTEO CASAS ROM, MAGDALENA G. AUGUIS, PILAR MASIN MATAS, JOVINA B. PELAYAO, TEODULO O. CARDENO, FIDEL G. LIBRE, PANFILO DINGAL ANIÑON, EDUARDO A. CORTEZ, VENANCIO B. CARIO, JONATHAN G. COMIDOY, EVERARDO L. BERNIR, CRISPIN B. SALUPAN, RUFINA A. VILLAHERMOSA, ANDREA G.A. PORLARES, NEMESIO C. GASCAL, VICENTE I. CARDENO, SAMUEL A. CREDO, LITA OPLINA QUIMPAN, RUPERTO G. QUINDOY, AGRIPINA SURDILLA, SIXTO B. DIEZ, FUENTES A. CORTEZ, ISIDRO P. MAKIWAG, INECITA B. BAYUD, TERESITA DAHUYLA, MAURICIO A. VELARDE, AUREO BASALAN, ANTONIO GATDULA, ISIDRO REPONTE, TEOFILO G. MELLIJOR, DIOSDADO L. BAYRON, ROMEO GITO, JR., ROQUE QUIÑONES, ANASTACIO DAHOYLA, PEDRO DELLOSA RUBILLAR, PEDRO T. OROYAN, EMETERIO VENTEDO BAUTISTA, PERLA MARQUEZ BAGUIO, ROGELIO PELAYO CATAPAN, REY BACHILLER ARAGON, LEOPOLDO P. DIORESMA, JEREMIAS SUDAY, DANIEL D. DARUNDAY, BONIFACIO FULGUERINAS, ANDRES C. PANTOJA, FELOMINO L. GETIZO, CRISPIN ABELLA, CRISTITA S. BAGUIO, JOSE S. CAYAPOS, GREGORIO C. ROM, MELQUIADES M. CHAVES, RAMIL C. AYCO, LUZVIMINDA V. OMBING, MARCELO F. BOLOTAULO, ANTONIO DE LOS REYES, FERNANDO R. QUIÑO, TEOFILA FLORES, ROLANDO DELMO, JULIANA V. ACUÑA, VICTORINA A. CAMINADE, MIGUEL M. VILLEGAS, BONIFACIO A. ALCONTIN, AQUILINO C. BUZON, APARICIO A. MONTAÑA, EDUARDO RACOMA, CONCHITA RECEDE VALLE, ROQUE T. CHAVEZ, CESAR COLIS DONOS, CARLITO VILLANCIO, ESTRELLA CARCELLER, FELIPE A. ALO, CESO G. RANGAS, BERTOLDO S. LLAMERA, ARCADIO ACALA, LETECIA B. OUANO, TOMAS B. RUBILLAR, GERARDO C. DOONG, ELIZA JANE C. GILLANO, ROMUALDO CRUZ, MAMERTO F. SURDILLA, LEONARDO V. ORBETA, JUSTINA V. FROILAN, FERMIN R. CABALLERO, DOMINGO M. MANSALAY, REYNALDO D. SURDILLA, ROSITA C. LUNA, JERRY A. SUDAY, MIGUEL O. PADRIGON, CRISANTA CABALLES, ARMANDO L. RELAMPAGOS, HERMAN E. RECOMA, JOSE G. MARTINEZ, DOMINADOR L. CARTILLAS, JOSEFINA C. BUSANO, REMEDIOS Y. NAVALES, ESTANISLAO A. CARDONA, and SILVINO DE LOS SANTOS, Petitioners-Appellants, v. TROPICAL HOMES, INC., Respondent-Appellee.
DE LEON, JR., J.:
These two (2) consolidated petitions for review on certiorari, filed under Rule 45 of the Rules of Court, seek the reversal of the Decision 1 of the Court of Appeals in CA-G.R. SP No. 46262 dated August 5, 1998. However, while petitioners in G.R. No. 136827 entitled "Secretary of Agrarian Reform, Et. Al. v. Tropical Homes, Inc." also pray for a reversal of the appellate court's Resolution 2 dated October 8, 1998 denying their motion for reconsideration, the petitioners-appellants in G.R. No. 136799 entitled "Secretary of Agrarian Reform, Et. Al. v. Tropical Homes, Inc.", pray that the Resolution 3 dated November 10, 1998 of the appellate court ordering their motion for reconsideration expunged from the rollo, be set aside.
The Comprehensive Agrarian Reform Program (CARP) is the bastion of social justice of poor landless farmers, the mechanism designed to redistribute to the underprivileged the natural right to toil the earth, and to liberate them from oppressive tenancy. To those who seek its benefit, it is the means towards a viable livelihood and ultimately, a decent life. The objective of the State is no less certain: "landless farmers and farmworkers will receive the highest consideration to promote social justice and to move the nation toward sound rural development and industrialization." 4 Unfortunately, these two (2) related cases leave us in a serious predicament. For while we sympathize with the economically wanting, especially the landless farmers, we cannot go against what is laid down in our statute books and in established jurisprudence. Thus, we resolved to deny both petitions.chanrob1es virtua1 1aw 1ibrary
Carlos Iñigo is the former registered owner of parcels of land covered by TCT Nos. 30843, 30844, 30845 and 30846 located in Bago Iñigo, Toril, Davao City, with an aggregate area of more or less One Million Five Hundred Thirty-Two Thousand Four Hundred Fifteen (1,532,415) square meters.
On July 17, 1971, Iñigo and herein respondent Tropical Homes, Inc. (TROPICAL for brevity) entered into a Joint Venture Agreement for the development of the property into a residential area, which was later known as the "Better Living Subdivision" .
Inasmuch as the property was located in an agricultural zone, TROPICAL filed with the City Council of Davao an application for reclassification of the area from agricultural into residential.
On October 2, 1972, the City Council of Davao, through Resolution No. 558, 5 declared the site of the Better Living Subdivision as residential area, maintaining that it was outside the present Zonification and Development Plan of the City.
On February 14, 1975, Rosita M. Iñigo, by then the widow of Carlos Iñigo, together with the rest of the heirs of the late Carlos Iñigo, divided among themselves the properties above-mentioned through a Deed of Extra-Judicial Partition. This Deed was inscribed in the Register of Deeds of Davao City. As a result, TCT Nos. 30843, 30844, 30845 and 30846 were cancelled and in lieu thereof, TCT Nos. 47427, 47428, 47429 and 47430 were issued in their names.chanrob1es virtua1 1aw 1ibrary
On May 31, 1977, the Joint Venture Agreement dated July 17, 1971 entered into by the late Carlos Iñigo and respondent Tropical was also inscribed in the Registry of Deeds of Davao City. Coupled with the Notice and Manifestation of Conformity of the Heirs of the late Carlos Iñigo, TCT Nos. 47427, 47428, 47429 and 47430 were cancelled and replaced by TCT Nos. 56940, 56941, 56942 and 56943, all registered in the name of TROPICAL.
On August 29, 1990, the Department of Agrarian Reform (DAR), through its Davao City office, notified respondent Tropical that its property would be covered by the CARP.
On April 25, 1991, DAR issued three (3) Notices of Acquisition to TROPICAL, specifying that One Million Thirty-Seven Thousand Two Hundred Seventy-Two (1,037,272) square meters of the land covered by TCT Nos. 56940, 56941, 56942 and 56943 would be the subject of compulsory acquisition.chanrob1es virtua1 1aw 1ibrary
This landholding is what is now involved in the present controversy.
Following the issuance of the corresponding Notices of Valuation, the DAR Regional Director instructed the Register of Deeds of Davao City to cancel the titles of three (3) separate parcels of land consisting of an area of One Million Thirty-Seven Thousand Two Hundred Seventy-Two (1,037,272) square meters, the area subject to compulsory acquisition. Thereafter, TCT No. T-184249 was issued in the name of the Republic of the Philippines.
Consequently, DAR, through Certificate of Land Ownership Award (CLOA) No. 301148, distributed the landholding to the identified farmer-beneficiaries.
On November 17, 1993, TROPICAL filed a petition with the Provincial Agrarian Reform Adjudicator (PARAD) 6 for the cancellation of the CLOA mainly on the ground that the landholding was outside the coverage of the CARP.
While the petition was pending, a Motion For Intervention 7 was filed by Rolando B. Bersamin, Gaudencio O. Basa, Henry Cabrera, Rolando A. Bersamin II, Isidora Fallorina, Rodrigo Chavez, Arnel Dahoyla, Sandro Severino, Bellano Pacyao, Genara Diez and Eddie Maniego, all of whom alleged that they are bona fide residents of the landholding but were excluded in the CLOA.chanrob1es virtua1 1aw 1ibrary
In a Decision 8 dated May 6, 1997, the PARAD ruled in favor of TROPICAL. It also denied the motion for intervention, finding that the right over the property could be properly threshed out in a separate proceeding duly instituted for that purpose. Since their subsequent motion for reconsideration was similarly denied, the petitioners, as respondents in that case, filed a Notice of Appeal with the Department of Agrarian Reform Adjudication Board (DARAB) on May 30, 1997. Three (3) days later, they filed a Manifestation and Motion for the Issuance of a Temporary Restraining Order (TRO) and Writs of Preliminary Prohibitory and Mandatory Injunction with the same office, claiming that TROPICAL arrogated upon itself possessory rights over the property by causing the demolition of the farmers-beneficiaries' houses, fencing the property and posting guards to secure the area, in clear violation of the DARAB New Rules on Procedure. 9 DARAB issued an Order granting the motion. Moreover, in a Decision 10 dated December 4, 1997, DARAB reversed the ruling of the PARAD.chanrob1es virtua1 1aw 1ibrary
On December 11, 1997, TROPICAL filed a petition for review on certiorari with the Court of Appeals and an Urgent Motion for the Issuance of a TRO. It claimed that it would suffer irreparable injury if the execution of the assailed DARAB Decision was not enjoined; and that if petitioners continue demolishing the gates and the fence surrounding the land, unauthorized persons would be able to illegally enter and occupy it, bringing to naught all the time, effort and money consumed in clearing the area. 11 Subsequently, the appellate court granted the TRO prayed for, which was later replaced by a Writ of Preliminary Injunction.
On August 5, 1998, the Court of Appeals rendered its questioned Decision 12 in favor of TROPICAL. Both petitioners and petitioners-appellants filed their respective motions for reconsiderations. While the first motion was denied for having been filed beyond the fifteen (15) day reglementary period, the second motion for reconsideration was ordered expunged from the rollo, pursuant to the motion for partial reconsideration filed by TROPICAL. In that motion, it was alleged inter alia that petitioners-appellants are not parties to the case and that at no point in the whole legal process, from the PARAD to the Court of Appeals, were they allowed to intervene.
Hence, the present petitions.chanrob1es virtua1 1aw 1ibrary
The procedural infirmities of this case are replete, and sadly, fatal to both causes of action. In G.R. No. 136827, a careful review of the records reveals that the petition should have been dismissed outright for having been filed beyond the reglementary period to appeal. Petitioners claim that they received the Decision of the Court of Appeals dated August 5, 1998 on the 19th of the same month. 13 Thus, counting fifteen (15) days from August 19, 1998, their motion for reconsideration should have been filed on September 3, 1998. 14 However, what they filed instead was a Motion for Extension of Time 15 praying for an additional fifteen (15) days to file their motion for reconsideration. Unfortunately for petitioners, this Court has already ruled squarely on the matter that no such motion for extension shall be entertained. In the case of Habaluyas Enterprises, Inc. v. Japson, 16 we ruled that the fifteen (15) day reglementary period for appealing or for filing a motion for reconsideration cannot be extended. Petitioners argued that the Legal Assistance Division of the DAR Provincial Office in Davao City is undermanned because a substantial number of its staff is on official leave. Surely, this is an understandable excuse, albeit a non-legal one. We cannot go against what is settled in our jurisprudence by the mere expedient that there is not enough people to do the work. This is a problem that should be properly addressed by the executive branch of the government. The DAR must develop a system of procedure that would enable it to comply with the reglementary period for filing pleadings. 17 Apparently, petitioners erroneously assumed that the extension was granted considering that their motion for reconsideration was filed only on September 18, 1998, 18 or fifteen (15) days after the assailed Decision had become final and executory. In Rolloque, Et. Al. v. Court of Appeals, Et Al., 19 we already ruled in this wise —
The filing by petitioners of a motion for extension of time to file motion for reconsideration did not toll the fifteen (15) days period before a judgment becomes final and executory.
Since the decision of respondent Court of Appeals dated November 28, 1996 has long become final and executory at the time of the filing of this petition, this Court can no longer alter or modify the same.chanrob1es virtua1 1aw 1ibrary
Not having perfected their appeal in the manner and within the period fixed by law, the decision of the Court of Appeals had become final and executory. Such a failure carries with it the result that no court can exercise appellate jurisdiction to review the case. 20 However, it is true that we have recognized certain exceptions to this rule. In Ramos v. Bagasao, 21 we excused the delay of four (4) days in the filing of a notice of appeal because the questioned decision of the trial court was served upon appellant at a time when her counsel of record was already dead. 22 Her new counsel could only file the appeal four (4) days after the prescribed reglementary period was over. 23 In Republic v. Court of Appeals, 24 we allowed the perfection of an appeal by the Republic despite the delay of six (6) days to prevent a gross miscarriage of justice since it stood to lose hundreds of hectares of land already titled in its name and had since then been devoted for educational purposes. 25 In Olacao v. National Labor Relations Commission, 26 we accepted a tardy appeal considering that the subject matter in issue had theretofore been judicially settled, with finality, in another case. 27 The dismissal of the appeal would have had the effect of the appellant being ordered twice to make the same reparation to the appellee. 28 Unfortunately, we find no reason to make this case an exception. Our ruling in Habaluyas Enterprises, Inc. v. Japson 29 has been in force for fifteen (15) years. It is hard to believe that petitioners were not aware of this ruling, or assuming that they were, their utter disregard of it is simply unacceptable.
The petitioners-appellants in G.R. No. 136799 likewise committed a procedural error fatal to their cause of action. When they filed their Motion for Intervention on November 25, 1996, 30 the DARAB New Rules of Procedure was already in effect. 31 Rule IX, Sec. 3 thereof states —
SECTION 3. Intervention. — The filing of a motion for intervention shall be discouraged. Such motion shall be entertained only upon a clear showing by the would-be intervenor that he has a substantial right or interest in the case that cannot be adequately pursued and protected in another proceeding.chanrob1es virtua1 1aw 1ibrary
Thus, for such a motion for intervention to be entertained, two (2) requisites must concur. First, the would-be intervenor must show that he has a substantial right or interest in the case and that second, it cannot be adequately pursued and protected in another proceeding. The absence of even one requisite will warrant its denial. Acting on this provision, the PARAD in fact denied the motion for intervention, ruling that "their (petitioners-intervenors) rights over the property . . . can be properly threshed out in a separate proceeding duly instituted for the purpose." 32 In Republic v. Sandiganbayan, 33 we held that the discretion of a court (in this case a quasi-judicial agency) to allow intervention, once exercised, cannot be reviewed by certiorari nor controlled by mandamus save in instances where such discretion has been exercised in an arbitrary or capricious manner. Petitioners-appellants have not shown that the exercise of this discretion was made in the manner above-described. Hence, it behooves this Court to leave the denial of the motion for intervention to the wisdom of the PARAD. Besides, the theory of petitioners-appellants that as bona fide occupants of the landholding, they automatically acquire a substantial right or interest in the case 34 is unmeritorious. The (right or) interest here referred to is generally required to be direct and not consequential, and one properly determinable in the action in which intervention is sought. 35 The issue of whether or not they were improperly excluded from the CLOA is an issue totally different from that in G.R. No. 136827, which is whether the City Council of Davao, through Resolution No. 558, validly reclassified the landholding from agricultural area to residential area, hence, rendering it outside the coverage of the CARP. If indeed it was validly reclassified, then there would be no CLOA to speak of. Petitioners-appellants would have had no cause of action. Conversely, if the reclassification was invalid, then the CLOA's legality would merely be affirmed. It must be borne in mind that the alleged substantial right or interest of petitioners-appellants is based not on the legality or illegality of the CLOA brought about by the supposed questionable reclassification done by the City Council of Davao through Resolution No. 558, rather, it is based on their claim that they were improperly excluded from it. Thus, their interest is not one properly determinable in the action in which intervention is sought. To further complicate the case by adding parties who have totally separate interests which can be the proper subject of a separate proceeding, will simply delay the expeditious resolution thereof. It has been settled that the right to intervene is not an absolute right, for the statutory rules or conditions for the right to apply must be shown. 36 As the two (2) requisites were not met, petitioners-appellants have no standing to intervene. At this point, the proper course of action was simply to have filed a separate proceeding altogether.
Furthermore, the fact that petitioners-appellants were served with pleadings, resolutions, orders and decisions from the PARAD to this Court cannot be construed as an implied admission of their being parties to the case. Not even the Resolution 37 dated December 12, 1997 of the Court of Appeals requiring them to Comment on the Petition of TROPICAL, nor the Resolution 38 dated June 16, 1999 of this Court requiring them to Reply to the Comment 39 filed by the same respondent makes them parties. Intervention is merely collateral or accessory or ancillary to the principal action, and is not an independent proceedings. 40 By this process, a person not originally made a party may be permitted on his own application to obtain the status of a party to the principal action. 41 In other words, the only way for an intervenor to become a party of a case, is if a court or any other quasi-judicial agency authorized by law grants his motion to intervene. In the case at bar, petitioners-appellants failed to produce any evidence that would prove that their motion to intervene was granted. In fact, the records show that it was denied by the PARAD. The petitioners-appellants, not being parties to this case, and therefore having no legal standing to file the petition before us, their said petition must be denied.chanrob1es virtua1 1aw 1ibrary
Finally, even if petitioners-appellants could prove that they had every right to intervene, it is too late in the day to allow the same. The petitioners in G.R. No. 136827 failed to file their motion for reconsideration of the Decision 42 of the Court of Appeals within the reglementary period. Thus, it has become final and executory. Logically, as the case has already been terminated by final judgment, intervention is no longer possible. 43
It is indeed lamentable that the two (2) instant petitions must be denied for failure to comply with the procedural requirements set forth in the Rules of Court. While it is true that a litigation is not a game of technicalities, it is equally true that every case must be prosecuted in accordance with the prescribed procedure to ensure an orderly and speedy administration of justice. 44
WHEREFORE, in view of the foregoing, the consolidated petitions are hereby DENIED. The assailed Resolution dated November 10, 1998 of the Court of Appeals ordering petitioners-appellants' motion for reconsideration expunged from the rollo is hereby AFFIRMED.chanrob1es virtua1 1aw 1ibrary
Bellosillo, Mendoza and Quisumbing, JJ., concur.
Buena, J., abroad on official business.
1.	Penned by Associate Justice Jorge S. Imperial and concurred in by Associate Justices Ramon A. Barcelona and Demetrio G. Demetria (Third Division), Rollo, G.R. No. 136799, pp. 39-53.
2.	CA Rollo, p. 452.
4.	Declaration of Policies and Principles, Republic Act No. 6657:jgc:chanrobles.com.ph
"AN ACT INSTITUTING A COMPREHENSIVE AGRARIAN REFORM PROGRAM TO PROMOTE SOCIAL JUSTICE AND INDUSTRIALIZATION, PROVIDING THE MECHANISM FOR ITS IMPLEMENTATION, AND FOR OTHER PURPOSES."cralaw virtua1aw library
5.	Rollo, G.R. No. 136827, pp. 126-127.
6.	DARAB v. Court of Appeals, 266 SCRA 404, 419 (1997):jgc:chanrobles.com.ph
"The Department of Agrarian Reform's exclusive original jurisdiction is exercised through hierarchically arranged agencies, namely, the Department of Agrarian Reform Adjudication Board (DARAB), the Regional Agrarian Reform Adjudicator (RARAD) and the Provincial Agrarian Reform Adjudicator (PARAD). The latter two exercise "delegated authority," while the first exercises appellate jurisdiction over resolutions, orders, decisions and other dispositions of the RARAD and the PARAD, and "functional supervision" over the RARAD and the PARAD" .
7.	Annex "16" ; CA Rollo, pp. 351-353.
8.	Penned by Provincial Adjudication Damian L. Aninion, Annex "D", CA Rollo, pp. 51-62.
9.	Sec. 1 Rule XII provides;
Section 1.	Execution Upon Final Order or Decision.
Execution shall issue upon an order, resolution or decision that finally disposes of the action or proceeding. Such execution shall issue as a matter of course and upon the expiration of the period to appeal therefrom if no appeal has been duly perfected.
10.	Annex "A" ; CA Rollo, pp. 28-43.
11.	CA Rollo, p. 103.
12.	Supra, note 1.
13.	Motion for Reconsideration, CA Rollo, p. 442.
14.	Rule 52 of the New Rules on Civil Procedure state —
SECTION 1.	Period of filing. — a party may file a motion for reconsideration of a judgment or final resolution within fifteen (15) days from notice thereof, with proof of service on the adverse party.
16.	142 SCRA 208, 212 (1986).
"Beginning one month after the promulgation of this Resolution, the rule shall be strictly enforced that no motion for extension of time to file a motion for new trial or reconsideration may be filed with the Metropolitan or Municipal Trial Courts, the Regional Trial Courts, and the Intermediate Appellate Court (now Court of Appeals). Such a motion may be filed only in cases pending with the Supreme Court as the court of last resort, which may in its sound discretion either grant or deny the extension requested."cralaw virtua1aw library
17.	Fortich v. Corona, 298 SCRA 678, 690 (1998).
18.	CA Rollo, pp. 447-448.
19.	193 SCRA 47, 56 (1991).
20.	Azores v. Securities and Exchange Commission, 252 SCRA 387; 388 (1996).
21.	96 SCRA 395 (1980).
22.	Bank of America, NT & SA v. Gerochi, Jr., 230 SCRA 9, 15 (1994).
23.	Id.
25.	Supra, note 22.
30.	Annex "16" ; CA Rollo, pp. 351-353.
31.	June 22, 1994 (Date of Effectivity).
32.	CA Rollo, p. 61.
35.	59 Am Jur 2d 592.
36.	Big Country Ranch Corp. v. Court of Appeals, 227 SCRA 161, 165 (1993).
38.	Rollo, G.R. No. 136799, p. 196-A.
39.	Rollo, G.R. No. 136799, p. 181.
40.	J.M. Tuason & Co., Inc. v. Torres, 105 SCRA 653, 673 (1981); Islamic Directorate of the Philippines, Et. Al. v. CA, Et Al., 272 SCRA 454, 467 (1997).
41.	59 Am Jur 2d 574, 575.
43.	Rabino v. Cruz, 222 SCRA 493, 501 (1993).
44.	Supra, note 17 at 691.


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\section{Introduction}

The precise measurements of the cosmic microwave background (CMB) anisotropies initiated the era of precision cosmology \citep{WMAP:2003elm,WMAP:2003ivt}. Nevertheless, with the improvement of measurement precisions of cosmological parameters, some tensions between the early- and late-universe observations arised.
In particular, the values of the Hubble constant inferred from the $Planck$ CMB observation (based on the $\Lambda$CDM model) \citep{Planck:2018vyg} and determined by the distance-ladder measurement (model-independent) \citep{Riess:2021jrx} are shown to be in more than $5\sigma$ tension \citep{Riess:2021jrx}, which is now commonly believed as a severe crisis for cosmology \citep{Riess:2019qba,Verde:2019ivm}. The Hubble tension is widely discussed in the literature \citep{Riess:2019qba,Verde:2019ivm,Guo:2018ans,Perivolaropoulos:2021jda,Gao:2021xnk,DiValentino:2021izs,Abdalla:2022yfr,Cai:2021wgv,Yang:2018euj,DiValentino:2020zio,DiValentino:2019jae,DiValentino:2019ffd,Liu:2019awo,Zhang:2019cww,Ding:2019mmw,Li:2020tds,Wang:2021kxc,Vagnozzi:2021tjv,Vagnozzi:2021gjh,Vagnozzi:2019ezj,Guo:2019dui,Vagnozzi:2019ezj,Feng:2019jqa,Lin:2020jcb,2022arXiv221213146G,2022arXiv221213433Z}. So far, there is no consensus on a valid extended cosmological model that can truly solve the Hubble tension. Therefore, some cosmological probes that can independently measure the Hubble constant need to be greatly developed. The gravitational wave (GW) standard siren method is one of the most promising options.

Different from the traditional electromagnetic (EM) observations, GW observations open a new window into exploring the expansion history of the universe. The GW waveform encodes the information of the luminosity distance, which is called a standard siren \citep{Schutz:1986gp,Holz:2005df}. Applying GW standard sirens in cosmology has recently been widely discussed in the literature \citep{Holz:2005df,Dalal:2006qt,Cutler:2009qv,Bian:2021ini,Cai:2016sby,Cai:2017aea,Cai:2017plb,Zhang:2019ylr,Chen:2020dyt,Gray:2019ksv,Zhao:2010sz,Zhao:2018gwk,Du:2018tia,Cai:2018rzd,Yang:2019bpr,Yang:2019vni,Bachega:2019fki,Chang:2019xcb,He:2019dhl,Zhao:2019gyk,Wang:2021srv,Qi:2021iic,Jin:2021pcv,Zhu:2021bpp,deSouza:2021xtg,2022arXiv220100607W,2022arXiv220209726W,Jin:2022tdf,2022arXiv221110087H,2022arXiv220813999C,Wang:2022rvf,2022arXiv221213183D,2022arXiv220303956C,2022arXiv221200531S,Cao:2021zpf,Leandro:2021qlc,Fu:2021huc,Ye:2021klk,Chen:2020zoq,Mitra:2020vzq,Hogg:2020ktc,Nunes:2020rmr,Borhanian:2020vyr,2022arXiv220211882J,Jin:2020hmc}. If the redshift information of the GW source could be obtained by identifying the EM counterparts (we usually refer to this kind of GW standard sirens as bright sirens), the distance-redshift relation could be established for cosmological parameter estimations. While for the GW events without EM counterparts, the statistical analysis of the GW event associated with the galaxy catalog can also be applied in obtaining the redshift information (we usually refer to this kind of GW standard sirens as dark sirens).

In fact, the frequency ranges of GW standard sirens are wide (from nanohertz to a few hundred hertz), corresponding to different GW sources. Aiming at detecting GWs in different frequency bands, the pulsar timing arrays (PTAs), the space-based GW detectors, and the ground-based GW detectors are proposed.

The nanohertz GWs emitted by the supermassive black hole binaries (SMBHBs) could be detected by PTA, a natural Galactic-scale detector of millisecond pulsars (MSPs). Although it is difficult to detect GWs from individual SMBHBs by the current PTA projects, e.g., the European Pulsar Timing Array \citep{Kramer:2013kea}, the North American Nanohertz Observatory for Gravitational Waves \citep{McLaughlin:2013ira}, and the Parkes Pulsar Timing Array (Australia) \citep{Hobbs:2013aka}, it is expected that the individual SMBHBs could be detected by the SKA-era PTAs \citep{Smits:2008cf}. \citet{2020ApJ...889...79Y} proposed that the currently available SMBHB candidates with known redshift could be detected by the future SKA-era PTAs, allowing SMBHBs to be treated as standard sirens to explore the cosmic expansion history. \citet{2022arXiv220100607W} forecasted the cosmological parameter estimation with the bright sirens and dark sirens of individual SMBHBs with the SKA-era PTAs.

The space-based GW detectors are proposed to detect GWs emitted from the massive black hole binaries (MBHBs) in the millihertz frequency band, e.g., Taiji \citep{Wu:2018clg,Ruan:2018tsw,Hu:2017mde}, TianQin \citep{Luo:2020bls,Milyukov:2020kyg,TianQin:2020hid}, and the Laser Interferometer Space Antenna \citep{2017arXiv170200786A,2022arXiv220405434A}. The space-based GW detectors could detect high-redshift GW events (up to $z\simeq 15-20$), which are expected to provide high-redshift GW standard siren data. Some works show that the EM signals could be emitted in the process of MBHB mergers in both the radio and optical bands \citep{Palenzuela:2010nf,OShaughnessy:2011nwl,Moesta:2011bn,Kaplan:2011mz,Shi:2011us,Blandford:1977ds,Meier:2000wk,Dotti:2011um}. Applying these bright sirens in cosmological parameter estimation has been forecasted in the literature \citep{Zhao:2019gyk,Wang:2019tto,Wang:2021srv,Zhu:2021bpp,Zhu:2021aat,2022arXiv220405434A,Mangiagli:2022elu,Tamanini:2016uin,Caprini:2016qxs}.

The ground-based GW detectors could observe stellar-mass binaries in the frequency band of a few hundred hertz.
The only multi-messenger observation event GW170817 from a binary neutron star (BNS) merger gave the first measurement of the Hubble constant using the standard siren method with a $14\%$ precision \citep{LIGOScientific:2017adf}. The measurement precision of the Hubble constant could reach $2\%$ using 50 similar GW standard sirens \citep{Chen:2017rfc}, showing the potential of standard siren method in cosmological parameter estimation. In the next decades, the third-generation (3G) ground-based GW detectors, the Cosmic Explorer (CE) in the U.S. \citep{LIGOScientific:2016wof} and the Einstein Telescope (ET) in Europe \citep{Punturo:2010zz} will observe a large number of GW events in a wide range of redshift because the sensitivities of them are one order of magnitude improved over the current detectors \citep{2021arXiv210909882E}.

In the next decades, it is expected that we could obtain the multi-band GW standard siren data. Owing to the fact that the numbers of detectable GWs and signal-to-noise ratios (SNRs) in different frequency bands are different, the joint future multi-band GW standard siren observations are expected to play an important role in cosmological parameter estimation.

In this work, the first question to be answered is what precision the cosmological parameters could be measured to by the joint constraints of future multi-band GW standard siren observations. The second question we wish to answer is what role the multi-band GW standard sirens could play in breaking cosmological parameter degeneracies generated by the EM observations. Note that, in this work, we only focus on the GW bright standard siren observations. We will consider the future bright siren observations from the SKA-era PTAs, the space-based GW detectors, and the 3G ground-based GW detectors, which are in different frequency bands, and constrain the cosmological parameters relevant to dark energy and the Hubble constant issues using the mock data of joint multi-band GW standard sirens.

The paper is organized as follows. In Section~\ref{simulation:PTA}, we introduce the method of simulating GW standard sirens from the SKA-era PTA. In Section~\ref{simulation:Taiji}, we introduce the method of simulating GW standard sirens from Taiji. In Section~\ref{simulation:CE}, we introduce the method of simulating GW standard sirens from CE.
In Section~\ref{results}, we give the constraint results and make some relevant discussions. The conclusion is given in Section~\ref{Conclusion}.

\section{Method}

\subsection{Simulation of GW standard sirens from SKA-era PTAs}\label{simulation:PTA}
For the simulations of nanohertz GWs, following \citet{2020ApJ...889...79Y} and \citet{2022arXiv220100607W}, we choose the currently available SMBHB candidates with known redshifts and analyze the ability of SKA-era PTAs to detect them.

GW signals are detected in the timing residuals of MSPs by removing model-predicted times of arrival (ToAs) from the observational ToA data. The time residuals induced by a single GW source measured at time $t$ on the Earth can be written as
\begin{align}
s(t,\hat{\Omega}_{\rm s},\hat{\Omega}_{\rm p})=F_{+}(\hat{\Omega}_{\rm s},\hat{\Omega}_{\rm p})\Delta A_+(t)+F_{\times}(\hat{\Omega}_{\rm s},\hat{\Omega}_{\rm p})\Delta A_{\times}(t),
\end{align}
where $\hat{\Omega}_{\rm s}$ and $\hat{\Omega}_{\rm p}$ are the unit vectors pointing from the GW source and pulsar to the observer, respectively. $F_+(\hat{\Omega}_{\rm s},\hat{\Omega}_{\rm p})$ and $F_\times(\hat{\Omega}_{\rm s},\hat{\Omega}_{\rm p})$ are the antenna response functions and take the forms \citep{Wahlquist:1987rx}
\begin{align}
F_+(\hat{\Omega}_{\rm s},\hat{\Omega}_{\rm p})=&\frac{1}{4(1-\cos\delta)}\Big\{(1+\sin^2\beta_{\rm s})\cos^2\beta_{\rm p} \nonumber\\
                              &\times \cos[2(\alpha_{\rm s}-\alpha_{\rm p})]-\sin2\beta_{\rm s}\sin2\beta_{\rm p}\cos(\alpha_{\rm s}-\alpha_{\rm p})
\nonumber\\
                              &+\cos^{2}\beta_{\rm s}(2-3\cos^{2}\beta_{\rm p})\Big\},\nonumber\\
F_\times(\hat{\Omega}_{\rm s},\hat{\Omega}_{\rm p})=&~~\frac{1}{2(1-\cos\delta)}\Big\{\cos\beta_{\rm s}\sin2\beta_{\rm p}\sin(\alpha_{\rm s}-\alpha_{\rm p}) \nonumber\\
                              &- \sin\beta_{\rm s}\cos^2\beta_{\rm p}\sin[2(\alpha_{\rm s}-\alpha_{\rm p})\Big\},
\end{align}
where $(\alpha_{\rm s},\beta_{\rm s})$ and $(\alpha_{\rm p},\beta_{\rm p})$ are the right ascension and declination of the GW source and pulsar. $\delta$ is the opening angle between the GW source and pulsar with respect to the observer,
\begin{equation}
\cos\delta=\cos\beta_{\rm s}\cos\beta_{\rm p}\cos(\alpha_{\rm s}-\alpha_{\rm p})+\sin\beta_{\rm s}\sin\beta_{\rm p}.
\end{equation}

The forms of $\Delta A_{+,\times}(t)$ are given by
\begin{equation}
\centering
\Delta A_{+,\times}(t)=A_{+,\times}(t)-A_{+,\times}(t_{\rm p}),
\end{equation}
where $t_{\rm p}$ is the time at which GW passes the MSP,
\begin{equation}
t_{\rm p}=t-d_{\rm p}(1-\cos\delta)/c,
\end{equation}
with $d_{\rm p}$ the pulsar distance. For the SMBHBs in circular orbits, $A_{+,\times}(t)$ can be expressed as
\begin{align}
A_+(t)=&\frac{h_0(t)}{2\pi f(t)}\Big\{(1+\cos^2\iota)\cos2\psi\sin[\phi(t)+\phi_0]\nonumber\\
                              &~~+ 2\cos\iota\sin2\psi\cos[\phi(t)+\phi_0]\Big\},
                              \nonumber\\
A_\times(t)=&\frac{h_0(t)}{2\pi f(t)}\Big\{(1+\cos^2\iota)\sin2\psi\sin[\phi(t)+\phi_0] \nonumber\\
                              &~~- 2\cos\iota\cos2\psi\cos[\phi(t)+\phi_0]\Big\},
\end{align}
where $\psi$ is the GW polarization angle, $\phi_{0}$ is a phase constant, and $\iota$ is the inclination angle of the binary orbit. Assuming SMBHBs inspiral in circular orbits, the GW strain amplitude $h(t)$ is given by
\begin{align}
h(t)=2\frac{(G\mathcal M_{\rm c})^{5/3}}{c^{4}}\frac{[\pi f(t)]^{2/3}}{d_{\rm L}}.
\end{align}

The frequencies and phases of GWs can be described as
\begin{align}
f(t)=\Big[f_{0}^{-8/3}-\frac{256}{5}\pi^{8/3}\Big(\frac{G\mathcal{M}_{\rm c}}{c^{3}}\Big)^{5/3}t\Big]^{-3/8},
\end{align}
\begin{align}
\phi(t)=\frac{1}{16}\Big(\frac{G\mathcal{M}_{\rm c}}{c^{3}}\Big)^{-5/3}\Big\{(\pi f_{0})^{-5/3}-[\pi f(t)]^{-5/3}\Big\},
\end{align}
where $f_{0}=2f_{\rm orb}$ is the GW frequency at the time of our first observation, $\mathcal{M}_{\rm c}$ is the observed chirp mass, $M=m_1+m_2$ is the total mass of a binary system with the component masses $m_1$ and $m_2$, $\eta=m_1 m_2/(m_1+m_2)^2$ is the symmetric mass ratio, $f_{\rm orb}=(2\pi T)^{-1}$ is the orbit frequency, and $T$ is the orbital periods of SMBHB candidates taken from \citet{Valtonen:2008tx,Graham:2015gma,Graham:2015tba,Charisi:2016fqw,Yan:2015mya,Li:2016hcm,Zheng:2015dij,Li:2017eqf}. Here we calculate $f_{0}$ using the orbital periods of the 154 SMBHB candidates.

The SNR of the GW signal detected by a PTA is written as
\begin{align}
\rho^2=\sum_{i=1}^{N_{\rm p}}\sum_{n=1}^{N}\left[\frac{s_i(t_n)}{\sigma_{t,i}}\right]^2,
\end{align}
where $N_{\rm p}$ is the number of MSPs, $N$ is the total number of data points of each MSP, $s_{i}(t_{n})$ is the timing residual of $i$-th MSP at time $t_{n}$, and $\sigma_{t,i}$ is the root mean square (rms) timing residual of the $i$-th MSP. Here we set the threshold of SNR to be 8.

We use the Fisher information matrix to estimate measurement errors of $d_{\rm L}$. For a PTA containing $N_{\rm p}$ independent MSPs, the Fisher matrix is expressed as
\begin{align}
{F}_{ab}=\sum_{i=1}^{N_{\rm p}}\sum_{n=1}^{N}\frac{\partial{s_i(t_n)}}{\sigma_{t,i}\partial{\theta_a}}\frac{\partial{s_i(t_n)}}{\sigma_{t,i}\partial{\theta_b}},
\end{align}
where $\bm{\theta}$ denotes the free parameters to be estimated. Here, the Fisher matrix includes nine parameters, including eight GW source parameters ($d_{\rm L}$, $\mathcal{M}_{\rm c}$, $\alpha_{\rm s}$, $\beta_{\rm s}$, $\iota$, $\psi$, $\phi_{0}$, $f_{0}$) and the pulsar distance $d_{\rm p}$. The error of the parameter $\theta_a$ is calculated by $\Delta\theta_a=\sqrt{(F^{-1})_{aa}}$, i.e., $\sigma_{d_{\rm L}}^{\rm inst}=\Delta d_{\rm L}=\Delta\theta_1$. We wish to note that we consider $m_{1} = m_{2}$ in the simulation. Owing to the fact that the inclination angle $\iota$, the polarization angle $\psi$, and the initial phase $\phi_0$ of the SMBHB candidates are not known yet, we consider $\iota=90^{\circ}$, $\psi = 0$, and $\phi_0 = 0$ for these SMBHBs.

The measurement of $d_{\rm L}$ is also affected by the weak lensing and we adopt the form \citep{Tamanini:2016zlh,Speri:2020hwc,Hirata:2010ba}
\begin{align}
\sigma_{d_{\rm L}}^{\rm lens}(z)=&\left[1-\frac{0.3}{\pi / 2} \arctan \left(z / 0.073\right)\right]\nonumber\\
&\times d_{\rm L}(z)\times 0.066\bigg[\frac{1-(1+z)^{-0.25}}{0.25}\bigg]^{1.8}.\label{lens}
\end{align}

The total error of $d_{\rm L}$ can be written as
\begin{align}
\sigma_{d_{\rm L}}=\sqrt{(\sigma_{d_{\rm L}}^{\rm inst})^2+(\sigma_{d_{\rm L}}^{\rm lens})^2}.
\end{align}

Here we note that the ability of PTA GW observations is affected by many factors, for example, the number of MSPs $N_{\rm p}$ and rms of time residual $\sigma_t$. It is found that about 100 high-quality MSPs are sufficient for the detection of nanohertz GWs from individual SMBHBs \citep{2022arXiv220100607W}. {The current PTAs usually contain dozens of MSPs. In the future, we can expect SKA and FAST to observe hundreds of MSPs.} In the present work, we simulate 200 pulsars to detect nanohertz GWs. For the rms of timing residual, it consists of white noise and red noise.
Recent analysis shows that the total white noises of pulsars {could approach} 10--50 ns \citep{Porayko:2018sfa} in the SKA era, thus we consider the $\sigma_{t}$ to be $\sigma_{t}=20$ ns.
{SMBHB candidates usually emit GWs in the frequency range of $10^{-7}$--$10^{-8}$ Hz. In this frequency,} the red noise can be attenuated to a low noise level, and it does not affect the single GW detection, so it can be ignored.
{In addition, the stochastic gravitational wave background (SGWB) will also affect the detection of SMBHBs. However, recent studies have shown that SGWB is likely to be detected in about ten years. The SGWB can be regarded as red noise, which has slight impact in the frequency of $10^{-7}$--$10^{-8}$ Hz.}
Following \citet{2022arXiv220100607W}, we assume that the ToA data are obtained by monitoring the MSPs with the typical cadence of two weeks and the observation time is 10 years.
Based on the simulation method introduced above, 35 standard sirens could be detected by the SKA-era PTA. The standard siren data are shown in Fig.~\ref{Fig1}.

\subsection{Simulation of GW standard sirens from Taiji}
\label{simulation:Taiji}
In this section, we focus on the GW signal from the inspiral of a non-spinning MBHB that could be modeled by the restricted post-Newtonian (PN) waveform. For Taiji, the GW strain $h(t)$ can be described by two independent polarizations ${h_{+,\times}}(t)$ in the transverse-traceless gauge,
\begin{align}
 h(t) = {F_ + }(t;\theta ,\phi ,\psi ){h_ + }(t) + {F_ \times }(t;\theta ,\phi ,\psi ){h_ \times }(t),
\end{align}
where $F_{+,\times}$ are antenna response functions, ($\theta$, $\phi$) denote the location of the GW source.
We can separate the antenna response function into a polarization angle part and a $D_{+,\times}$ part that describes the dependence of time,
\begin{eqnarray}
 F_{+}^{(1)}(t) &=& \frac{1}{2}\Big({\rm cos}(2\psi)D_{+}(t)-{\rm sin}(2\psi)D_{\times}(t)\Big),  \\
 F_{\times}^{(1)}(t) &=& \frac{1}{2}\Big({\rm sin}(2\psi)D_{+}(t)+{\rm cos}(2\psi)D_{\times}(t)\Big)  .
\end{eqnarray}

For the inspiral process, the specific forms of $D_{+,\times}$ with low-frequency approximation are given in \citet{2019arXiv190907104R},
\begin{align}
D_{+}(t) =& \frac{\sqrt{3}}{64}\bigg[-36{\rm sin}^2\theta\,{\rm sin}\big(2\alpha(t)-2\beta\big)+\big(3+{\rm cos(2\theta)}\big)\nonumber \\
&\times\bigg({\rm cos}(2\phi)\Big(9\sin(2\beta)-{\rm sin}\big(4\alpha(t)-2\beta\big)\Big)\nonumber \\
&+{\rm sin}(2\phi)\Big({\rm cos}\big(4\alpha(t)-2\beta\big)-9\cos(2\beta)\Big)\bigg)\nonumber \\
&-4\sqrt{3}{\rm sin}(2\theta)\Big({\rm sin}\big(3\alpha(t)-2\beta-\phi\big)-3{\rm sin}\big(\alpha(t)\nonumber \\
&-2\beta+\phi\big)\Big)\bigg],  \\
D_{\times}(t) =& \frac{1}{16}\bigg[\sqrt{3}{\rm cos}\theta\Big(9{\rm cos}(2\phi-2\beta)-{\rm cos}\big(4\alpha(t)-2\beta\nonumber \\
&-2\phi\big)\Big)-6{\rm sin}\theta\Big({\rm cos}\big(3\alpha(t)-2\beta-\phi\big)\nonumber \\
&+3{\rm cos}\big(\alpha(t)-2\beta+\phi\big)\Big)\bigg],
\end{align}
where $\alpha=2\pi f_{m}t+\kappa$ is the orbital phase of the guiding center, $\kappa$ is the initial ecliptic longitude of the guiding center, and $f_m=1/\rm yr$. We simply set $\beta=0$ in the simulation. The triangular GW detector Taiji can be equivalent to two independent L-shaped interferometers. The second interferometer is equivalent to the first one rotated by $45^\circ$ and the other equivalent antenna function is $F^{(2)}_{+,\times}(t;\theta,\phi,\psi)=F^{(1)}_{\times,+}(t;\theta,\phi-45^\circ,\psi)$.

In order to describe the GW signal in Fourier space, we replace the observation time $t$ with \citep{Buonanno:2009zt,Krolak:1995md}
\begin{align}
t(f)=t_{\rm c}-\frac{5}{256}\mathcal{M}^{-5/3}_{\rm c}(\pi f)^{-8/3},
\end{align}
where $t_{\rm c}$ is the coalescence time of MBHB.
The Fourier transformation of the strain can be obtained, i.e.,
\begin{eqnarray}
\tilde{h}(f)=-\left(\frac{5\pi}{24}\right)^{1/2}\mathcal{M}^{5/6}_{\rm c}\left[\frac{(\pi f)^{-7/6}}{D_{{\rm eff}}}\right] e^{-i\Psi}.
\end{eqnarray}
The effective luminosity distance, $D_{\rm eff}$, is defined as
\begin{equation}
D_{{\rm eff}}=d_{\rm L} \left[F^{2}_{+}\left(\frac{1+{\rm cos}^2 \iota}{2}\right)^2+F^{2}_{\times} {\rm cos}^2 \iota
\right]^{-1/2},
\end{equation}
where the form of $\Psi$ can refer to \citet{2019arXiv190907104R}.

The SNR of Taiji can be calculated by
\begin{equation}
\rho=\sqrt{\sum_{i=1}^{N}(\rho_i)^2},\label{rho}
\end{equation}
where $\rho_i=\sqrt{\left\langle\tilde{h_i},\tilde{h_i}\right\rangle}$. The inner product is defined as
\begin{align}
\left\langle a,b\right\rangle=4\int_{f_{\rm lower}}^{f_{\rm upper}}\frac{a(f)b^{*}(f)+a^{*}(f)b(f)}{2}\frac{df}{S_{\rm n}(f)},
\end{align}
where $f_{\rm lower}=10^{-4}$ Hz and $f_{\rm upper}=c^{3}/6\sqrt{6}\pi GM_{\rm obs}$ with $M_{\rm obs}=(m_{1}+m_{2})(1+z)$ \citep{Feng:2019wgq}.
Taiji's PSD is taken from \citet{Ruan:2018tsw}. We set the threshold of SNR to be 8 in the simulation.

For a network with $N$ independent interferometers, the Fisher matrix can be written as
\begin{equation}
F_{ij}=\sum_{n=1}^{N}\left\langle\frac{\partial\tilde{h}^{(n)}(f)}{\partial \theta_i},  \frac{\partial\tilde{h}^{(n)}(f)}{\partial \theta_j}\right\rangle,
\end{equation}
where $\bm{\theta}$ denotes nine GW source parameters ($d_{\rm L}$, $\mathcal{M}_{\rm c}$, $\eta$, $t_{\rm c}$, $\psi_{\rm c}$, $\iota$, $\theta$, $\phi$, $\psi$). The instrumental error of the luminosity distance is $\sigma_{d_{\rm L}}^{\rm inst}=\Delta d_{\rm L}=\sqrt{(F^{-1})_{11}}$.

We use Eq.~(\ref{lens}) to calculate the weak-lensing error.
The error caused by the peculiar velocity of the GW source is given by \citep{Kocsis:2005vv}
\begin{equation}
\sigma_{d_{\rm L}}^{\rm pv}(z)=d_{\rm L}(z)\times \bigg[ 1+ \frac{c(1+z)^2}{H(z)d_{\rm L}(z)}\bigg]\frac{\sqrt{\langle v^2\rangle}}{c},
\end{equation}
where $H(z)$ is the Hubble parameter and $\sqrt{\left\langle v^{2}\right\rangle}$ is the peculiar velocity of the GW source. In this work, we set $\sqrt{\left\langle v^{2}\right\rangle}=500$ km $\cdot$ s$^{-1}$.

In addition, for spectral sources whose redshifts can be determined at $z<2$, we assume that this error is trivial, so the redshift error $\sigma^{\rm reds}_{d_{\rm L}}$ can be ignored. However, for the GW events at $z>2$, the spectral redshifts in this range can hardly be obtained \citep{Dahlen:2013fea,Speri:2020hwc}. Thus, the redshift error should be taken into account. We estimate the error on the redshift measurement as $(\Delta z)_{n}\approx 0.03(1+z_{n})$ \citep{Dahlen:2013fea,Ilbert:2013bf} and propagate it to the error on $d_{\rm L}$,
\begin{align}
\sigma^{\rm reds}_{d_{\rm L}}=\frac{\partial d_{\rm L} }{\partial z}(\Delta z)_{n},
\end{align}
where $n$ represents the $n$th GW event.

The total error of $d_{\rm L}$ can be written as
\begin{align}
\sigma_{d_{\rm L}}&=\sqrt{(\sigma_{d_{\rm L}}^{\rm inst})^2+(\sigma_{d_{\rm L}}^{\rm lens})^2+(\sigma_{d_{\rm L}}^{\rm pv})^2+(\sigma_{d_{\rm L}}^{\rm reds})^2}.
\end{align}

Owing to the fact that the origin of MBHs is currently unclear, there is uncertainty in predicting the event rate of MBHBs. Based on a semianalytical galaxy formation model, three population models of MBHBs, the pop III, Q3d, and Q3nod models are proposed. The three models have different mechanisms of seeding and delay. In this work, we choose the pop III model as a representative to simulate standard sirens. Some works show that the EM signals could be emitted in the process of MBHB mergers in both the radio and optical bands \citep{Palenzuela:2010nf,OShaughnessy:2011nwl,Moesta:2011bn,Kaplan:2011mz,Shi:2011us,Blandford:1977ds,Meier:2000wk,Dotti:2011um}. Recent works predicted the number of GW detected by space-based GW observatory whose EM counterparts could also be detected by ELT and SKA \citep{Tamanini:2016zlh,Wang:2021srv,Yang:2021qge,Mangiagli:2022niy,Mangiagli:2022elu}. Following the method introduced in \citet{Tamanini:2016zlh,Wang:2021srv,Yang:2021qge,Mangiagli:2022elu}, we simulate the standard sirens based on the pop III model and obtain 28 bright sirens for 5-year observation of Taiji, which are shown in Fig.~\ref{Fig1}. The number is also basically consistent with that given in \citet{Wang:2021srv}.

For each simulated standard siren event, the sky location ($\theta$, $\phi$), the binary inclination $\iota$, the coalescence phase $\psi_{\rm c}$, and the polarization angle $\psi$ are evenly sampled in the ranges of $\cos\theta$ $\in$ $[-1, 1]$, $\phi$ $\in$ $[0, 360^{\circ}]$, $\cos\iota$ $\in$ $[-1, 1]$, $\psi_{\rm c}$ $\in$ [0, $ 360^\circ$], $\psi$ $\in$ [0, $360^\circ$], respectively. In this work, we assume $t_{\rm c}=0$ for simplicity. For the redshift and mass distributions of MBHBs, we use the numerical fitting formulas in \citet{Wang:2021srv} to fit the curves shown in Figure~3 of \citet{Klein:2015hvg}.

\subsection{Simulation of GW standard sirens from CE}
\label{simulation:CE}

In this work, we consider that all the GW standard sirens that can be detected by CE are the BNS mergers. The redshift distribution of BNS mergers adopts the form \citep{Zhao:2010sz,Cai:2016sby}
\begin{align}
P(z)=\frac{4\pi d_{\rm C}^{2}(z)R(z)}{H(z)(1+z)},
\end{align}
where the $(1+z)$ term arises from converting the source-frame time to the observor-frame time. $d_{\rm C}$ is the comoving distance. $R(z)$ describes the time evolution of the burst rate and takes the form \citep{Schneider:2000sg,Cutler:2009qv}
\begin{equation}
R(z)=\begin{cases}1+2 z, & z \leq 1, \\ \frac{3}{4}(5-z), & 1<z<5, \\ 0, & z \geq 5.\end{cases}
\end{equation}

In this work, we adopt the restricted Post-Newtonian (PN) approximation and calculate the waveform to the 3.5 PN order \citep{Sathyaprakash:2009xs,Blanchet:2004bb},
\begin{equation}
\tilde{h}(f)=\mathcal{A}f^{-7/6}\exp\{ i(2\pi ft_{\rm c}-\pi/4-2\psi_{\rm c}+2{\Psi}(f/2)-\varphi_{(2.0)})\},
\end{equation}
where the Fourier amplitude $\mathcal{A}$ is given by
\begin{align}
\mathcal{A}=&\frac{1}{d_{\rm L}}\sqrt{F_+^2\big(1+\cos^2(\iota)\big)^2+4F_\times^2\cos^2(\iota)}\nonumber\\
            &\times \sqrt{5\pi/96}\pi^{-7/6}\mathcal{M}_{\rm c}^{5/6},
\end{align}
and $\psi_{\rm c}$ is the coalescence phase. The detailed forms of $\Psi$ and $\varphi_{(2.0)}$ can refer to \citet{Zhao:2010sz}. The forms of $F_{+,\times}$ for CE are given by \citep{Sathyaprakash:2009xs}
\begin{align}
F_+(\theta, \phi, \psi)=&\frac{1}{2}\big(1 + {\cos ^2}(\theta )\big)\cos (2\phi )\cos (2\psi ) \nonumber\\
                              &~~- \cos (\theta )\sin (2\phi )\sin (2\psi ),\nonumber\\
F_\times(\theta, \phi, \psi)=&\frac{1}{2}\big(1 + {\cos ^2}(\theta )\big)\cos (2\phi )\sin (2\psi ) \nonumber\\
                              &~~+ \cos (\theta )\sin (2\phi )\cos (2\psi ),
\end{align}
where ($\theta$, $\phi$) are the angles describing the location of the source in the sky, and $\psi$ is the polarization angle.

We use Eq.~(\ref{rho}) to calculate the SNR of each GW event. For CE, $f_{\rm lower}=1$ Hz is the lower cutoff frequency and $f_{\rm upper}=2/(6^{3/2}2\pi M_{\rm obs})$ is the frequency at the last stable orbit with $M_{\rm obs}=(m_1+m_2)(1+z)$. We adopt the PSD of 40 km-arm-length CE.\footnote{\href{https://cosmicexplorer.org/sensitivity.html}{https://cosmicexplorer.org/sensitivity.html}} Here we set the threshold of SNR to be 8 in our simulation.

In this work, we consider three measurement errors of $d_{\rm L}$, including the instrumental error $\sigma^{\rm inst}_{d_{\rm L}}$, the weak-lensing error $\sigma^{\rm lens}_{d_{\rm L}}$, and the peculiar velocity error $\sigma^{\rm pv}_{d_{\rm L}}$. The total error of $d_{\rm L}$ is
\begin{align}
\sigma_{d_{\rm L}}=\sqrt{(\sigma_{d_{\rm L}}^{\rm inst})^2+(\sigma_{d_{\rm L}}^{\rm lens})^2+(\sigma_{d_{\rm L}}^{\rm pv})^2}.
\end{align}

\begin{figure}
\begin{center}
\includegraphics[width=0.45\textwidth]{fig1.pdf}
\caption{The simulated GW standard siren data points observed by PTA, Taiji, and CE. The yellow data points represent the 35 standard sirens from the 10-year observation of PTA, the red data points represent the 28 standard sirens from the 5-year observation of Taiji, and the blue data points represent the 1000 standard sirens from the 10-year observation of CE. The central values of the luminosity distances are calculated by the fiducial $\Lambda$CDM model based on the constraint results of $P lanck$ 2018 TT,TE,EE+lowE \citep{Planck:2018vyg}.}\label{Fig1}
\end{center}
\end{figure}

Recent forecasts show that the 3G ground-based GW detectors would detect $\mathcal{O}(10^5)$ BNS mergers per year, but only about $0.1\%$ of them have the detectable EM counterparts \citep{Yu:2021nvx}. \citet{Chen:2020zoq} recently showed that 910 GW standard sirens could be detected based on the 10-year observation of CE and Swift++. Therefore, in the forecast in the present work, we simulate 1000 GW standard sirens generated by BNS mergers based on the 10-year observation of CE.

For each simulated standard siren event, the masses of NSs ($m_{1}$, $m_{2}$) are randomly chosen in the ranges of [1, 2] $M_{\odot}$. Without loss of generality, the merger time is chosen to $t_{\rm c}=0$ in our analysis. The sky direction, binary inclination, polarization angle, and the coalescence phase are randomly chosen in the ranges of ${\rm cos}\,\theta\in [-1,1]$, $\phi\in [0,360^\circ]$, ${\rm cos}\,\psi\in [0,360^\circ]$, and $\psi_{\rm c}\in [0,360^\circ]$.
Here we note that the inclination angle should be randomly chosen in the range of $\cos\iota$ $\in$ $[-1, 1]$ when simulating isotropic GW sources. However, in this work, we assume that the redshifts of the GW events are determined by detecting SGRBs. Since SGRBs are strongly beamed, the detectable inclination angle is about $\iota\leq$ $20^{\circ}$ \citep{VERITAS:2021imb,Chen:2020zoq,Hirata:2010ba,Speri:2020hwc,Kocsis:2005vv,Rezzolla:2011da}. Therefore, in the present work, $\iota$ is randomly chosen in the range of $\iota\in [0,20^\circ]$.

In Fig.~\ref{Fig1}, we show the simulated standard siren data from PTA, Taiji, and CE. We can see that the number of standard sirens from CE is the largest, followed by PTA and Taiji. However, due to the fact that SNRs of GW events observed by CE are lower than those of PTA and Taiji, CE has the largest errors of luminosity distances at the same redshifts. The luminosity distance errors of PTA and Taiji are almost the same at similar redshifts.

\begin{table*}
\renewcommand\arraystretch{1.5}
\caption{The absolute errors (1$\sigma$) and the relative errors of the cosmological parameters in the $\Lambda$CDM, $w$CDM, and $w_{0}w_{a}$CDM models using the CMB, PTA, Taiji, CE, PTA+Taiji+CE, and CMB+PTA+Taiji+CE data. Here $H_0$ is in units of km s$^{-1}$ Mpc$^{-1}$.}\label{Tab1}
\centering
\normalsize
\setlength{\tabcolsep}{3mm}{
\begin{tabular}
{p{1.2cm}<{\centering} p{1.2cm}<{\centering} p{1.2cm}<{\centering} p{1.2cm}<{\centering} p{1.2cm}<{\centering} p{1.2cm}<{\centering} p{2.5cm}<{\centering} p{3.4cm}<{\centering}}
\hline\hline
Model & Error & CMB & PTA  & Taiji & CE  & PTA+Taiji+CE & CMB+PTA+Taiji+CE \\
\hline
 \multirow{4}{*}{$\Lambda$CDM}&  $\sigma(\Omega_m)$& 0.009 & 0.020 & 0.024 & 0.012 & 0.008 &0.003 \\
& $\sigma(H_0) $   & 0.61  & 0.49 & 0.70 & 0.45 & 0.29 &0.20\\
 & $\varepsilon(\Omega_m)$ &$2.7\%$ & $6.3\%$ & $11.7\%$ & $3.8\%$ & $2.8\%$  & $1.0\%$\\
  & $\varepsilon(H_0)$  &$0.9\%$ & $0.7\%$ & $1.6\%$ & $0.7\%$ & $0.5\%$ & $0.3\%$ \\
\hline
\multirow{6}{*}{$w$CDM}&  $\sigma(\Omega_m)$ & 0.058 & 0.038 & 0.033 & 0.017  & 0.015 & 0.003\\
  & $\sigma(H_0) $  & 6.30   & 2.25 & 1.75 & 0.95 & 0.69 & 0.37\\
& $\sigma(w) $  & 0.210 & 0.395 & 0.235 & 0.120 & 0.101 & 0.028 \\
 & $\varepsilon(\Omega_m)$ & $18.5\%$ & $11.8\%$ & $10.2\%$ & $5.4\%$ & $4.7\%$ & $1.0\%$ \\
  & $\varepsilon(H_0)$  & $9.1\%$    & $3.3\%$ & $2.6\%$ & $1.4\%$ & $1.0\%$ & $0.6\%$ \\
 & $\varepsilon(w)$   &$20.2\%$    & $31.9\%$ & $22.0\%$ & $11.8\%$ & $10.0\%$ & $2.8\%$ \\
\hline
 \multirow{7}{*}{$w_{0}w_{a}$CDM} &  $\sigma(\Omega_m)$ & 0.066 & 0.069 & 0.059 & 0.048 & 0.047 & 0.009\\
  & $\sigma(H_0) $  & 7.25   & 4.30 & 3.10 & 1.40 & 1.35 & 0.85 \\
 & $\sigma(w_{0}) $  & 0.605  & 0.750 & 0.530 & 0.220 & 0.195 & 0.110 \\
& $\sigma(w_{a})$ & 2.50 & 2.90 & 2.80 & 1.31 & 1.22 & 0.32\\
 & $\varepsilon(\Omega_m)$ &$20.6\%$ & $19.9\%$ & $16.9\%$ & $14.8\%$ & $14.8\%$ & $2.7\%$\\
  & $\varepsilon(H_0)$   & $10.6\%$   & $6.4\%$ & $4.7\%$ & $2.1\%$ & $2.0\%$ & $1.3\%$ \\
 & $\varepsilon(w_{0})$   & $112.0\%$   & $76.5\%$ & $74.6\%$ & $24.2\%$ & $21.0\%$  &$10.9\%$ \\
\hline\hline
\end{tabular}}
\end{table*}

\section{Results and discussion}\label{results}

\begin{figure*}
\includegraphics[width=0.4\textwidth]{fig2a.pdf
\includegraphics[width=0.4\textwidth]{fig2b.pdf
\caption{Constraints on the $\Lambda$CDM model. Left panel: Two-dimensional marginalized contours ($68.3\%$ and $95.4\%$ confidence level) in the $\Omega_{\rm m}$--$H_0$ plane by using the PTA, Taiji, CE, and PTA+Taiji+CE data. Right panel: Two-dimensional marginalized contours ($68.3\%$ and $95.4\%$ confidence level) in the $\Omega_{\rm m}$--$H_0$ plane by using the CMB, PTA+Taiji+CE, and CMB+PTA+Taiji+CE data.}\label{Fig2}
\end{figure*}

In this section, we report the constraint results. We use the simulated GW standard siren data from PTA, Taiji, and CE to constrain the $\Lambda$CDM [$w(z)=-1$], $w$CDM [$w(z)=\rm constant$], and $w_0w_a$CDM [$w(z)=w_0+w_a z/(1+z)$] models by performing the Markov-chain Monte Carlo analysis \citep{Lewis:2002ah}. For the CMB data, we employ the ``$Planck$ distance priors'' from the $Planck$ 2018 observation \citep{Chen:2018dbv,Planck:2018vyg}. The $1\sigma$ and $2\sigma$ posterior distribution contours for the cosmological parameters of interest are shown in Figs.~\ref{Fig2}--\ref{Fig5} and the $1\sigma$ errors for the marginalized parameter constraints are summarized in Table~\ref{Tab1}. We use $\sigma(\xi)$ and $\varepsilon(\xi)$ to represent the 1$\sigma$ absolute and relative errors of the parameter $\xi$, with $\varepsilon(\xi)$ defined as $\varepsilon(\xi)=\sigma(\xi)/\xi$.

\begin{figure*}
\includegraphics[width=0.4\textwidth]{fig3a.pdf
\includegraphics[width=0.4\textwidth]{fig3b.pdf
\caption{Constraints on the $w$CDM model. Here we show the two-dimensional marginalized contours ($68.3\%$ and $95.4\%$ confidence level) in the $w$--$\Omega_{\rm m}$ (left panel) and $w$--$H_0$ (right panel) planes using the PTA, Taiji, CE, and PTA+Taiji+CE data.}\label{Fig3}
\end{figure*}

\begin{figure*}
\includegraphics[width=0.4\textwidth]{fig4a.pdf
\includegraphics[width=0.4\textwidth]{fig4b.pdf
\caption{Constraints on the $w$CDM model. Here we show the two-dimensional marginalized contours ($68.3\%$ and $95.4\%$ confidence level) in the $w$--$\Omega_{m}$ (left panel) and $w$--$H_{0}$ (right panel) planes using the CMB, PTA+Taiji+CE, and CMB+PTA+Taiji+CE data.}\label{Fig4}
\end{figure*}

We first focus on the constraint results for the $\Lambda$CDM model. In the left panel of Fig.~\ref{Fig2}, we show the constraint results in the $\Omega_{\rm m}$--$H_0$ plane by using the simulated PTA, Taiji, CE, and PTA+Taiji+CE data. As can be seen, CE contributes the most to the PTA+Taiji+CE results, followed by PTA and Taiji. This is because the number of simulated standard sirens from CE is much more than those of PTA and Taiji. Although the measurement errors of $d_{\rm L}$ for CE are large, the constraints on cosmological parameters are reduced statistically. Compared with Taiji, PTA has more lower-redshift data points ($z<2$), so PTA can better constrain the Hubble constant. Moreover, due to the different redshift intervals of the simulated PTA, Taiji, and CE data, their parameter degeneracy orientations are slightly different, so their combination could break cosmological parameter degeneracies.
The combination of PTA, Taiji, and CE gives $\sigma(\Omega_{\rm m})=0.008$ and $\sigma(H_0)=0.29$ km s$^{-1}$ Mpc$^{-1}$, which are $33.3\%$ [$(0.012-0.008)/0.012$] and $35.6\%$ [$(0.45-0.29)/0.45$] better than those of CE. In the right panel of Fig.~\ref{Fig2}, we can see that the contours of CMB and PTA+Taiji+CE show different orientations and thus the combination of them could break cosmological parameter degeneracies. The prime cause is that GW could measure $H_0$ better, so it could lead to a different degeneracy direction compared with CMB. The combination of CMB and PTA+Taiji+CE gives $\sigma(\Omega_{\rm m})=0.003$ and $\sigma(H_0)=0.20$ km s$^{-1}$ Mpc$^{-1}$, and the constraint precisions of $\Omega_{\rm m}$ and $H_0$ are $1.0\%$ and $0.3\%$, meeting the standard of precision cosmology. In general, the joint PTA+Taiji+CE data could tightly constrain the Hubble constant, and if combined with CMB, the measurement precisions of cosmological parameters could be greatly improved (better than or at least equal to $1\%$), due to the parameter degeneracies being broken.

In Figs.~\ref{Fig3}--\ref{Fig4}, we show the constraint results in the $w$--$\Omega_{\rm m}$ and $w$--$H_0$ planes for the $w$CDM model. As can be seen from Fig.~\ref{Fig3}, CE also contributes the most to the PTA+Taiji+CE data. However, the ability of Taiji to constrain cosmological parameters in the $w$CDM model is better than that of PTA. This is because Taiji has more high-redshift standard sirens than PTA, so Taiji can better constrain EoS parameter of dark energy $w$. Meanwhile, the combination of PTA, Taiji, and CE gives $\sigma(w)=0.101$, which is $15.8\%$ better than the constraint result by CE. In Fig.~\ref{Fig4}, we see that the parameter degeneracy orientations of CMB and PTA+Taiji+CE are almost orthogonal and thus the combination of them could not only break cosmological parameter degeneracies but also tremendously improve the cosmological parameter constraints. The addition of the PTA+Taiji+CE data could reduce the $1\sigma$ absolute error of $w$ by $86.7\%$, compared with CMB. Moreover, the combination of CMB and PTA+Taiji+CE gives $\sigma(w)=0.028$, which is comparable with the latest constraint result by the CMB+BAO+SN data \citep{Brout:2022vxf}.

\begin{figure*}[!htbp]
\includegraphics[width=0.4\textwidth]{fig5a.pdf
\includegraphics[width=0.4\textwidth]{fig5b.pdf
\caption{Constraints on the $w_0w_a$CDM model. Left panel: Two-dimensional marginalized contours ($68.3\%$ and $95.4\%$ confidence level) in the $w_0$--$w_a$ plane by using the PTA, Taiji, CE, and PTA+Taiji+CE data. Right panel: Two-dimensional marginalized contours ($68.3\%$ and $95.4\%$ confidence level) in the $w_0$--$w_a$ plane by using the CMB, PTA+Taiji+CE, and CMB+PTA+Taiji+CE data.}\label{Fig5}
\end{figure*}

In Fig.~\ref{Fig5}, we show the case for the $w_0w_a$CDM model in the $w_0$--$w_a$ plane. As can be seen from the left panel of Fig.~\ref{Fig5}, the constraint results are the same as those in the $w$CDM model, i.e., CE contributes the most, followed by Taiji and PTA. The joint PTA+Taiji+CE data could give $\sigma(w_0)=0.195$ and $\sigma(w_0)=1.22$, which are both better than the constraint results by the CMB data. Furthermore, in the right panel of Fig.~\ref{Fig5}, we see that the combination of CMB and PTA+Taiji+CE could also break the parameter degeneracies and thus significantly improve the cosmological parameter constraints. The joint CMB+PTA+Taiji+CE data give $\sigma(w_0)=0.110$ and $\sigma(w_a)=0.32$, which are $81.8\%$ [$(0.605-0.110)/0.605$] and $87.2\%$ [$(2.50-0.32)/2.50$] better than the results of CMB.

Our results show that the joint future multi-band GW standard siren observations would play a crucial role in cosmological parameter estimation. CE contributes the most to the PTA+Taiji+CE results since the number of standard sirens detected by CE is much more than those of PTA and Taiji. PTA has more lower-redshift ($z<2$) data. Taiji has more higher-redshift data. Hence, PTA offers better constraints in the $\Lambda$CDM model, while in the dynamical dark energy models, Taiji offers better constraints. The joint multi-band GW standard siren data show great potential in constraining the $\Lambda$CDM model. Moreover, the parameter degeneracy orientations of them are slightly different and thus the combination of them could break the cosmological parameter degeneracies. However, the joint constraints perform not well in the $w$CDM and $w_0w_a$CDM models. Fortunately, the joint PTA+Taiji+CE data have different parameter degeneracy orientations from CMB, so the combination of them could effectively break the parameter degeneracies and greatly improve constraint precisions of cosmological parameters. It can be concluded that the future multi-band GW observations are worth expecting in precisely measuring cosmological parameters and helping solve important cosmological problems.

\section{Conclusion}\label{Conclusion}
In this work, we explore the potential of the joint constraints on cosmological parameters using future multi-band GW standard siren observations. We simulated the multi-band standard siren data based on the 10-year observation of CE, the 5-year observation of Taiji, and the 10-year observation of the SKA-era PTA, and used mock data to constrain three typical cosmological models, i.e., the $\Lambda$CDM, $w$CDM, and $w_0w_a$CDM models.

We find that the joint PTA+Taiji+CE data could give tight constraints on the Hubble constant, with the constraint precision being $0.5\%$ in the $\Lambda$CDM model. However, the joint data perform not well in constraining EoS parameters of dark energy. Fortunately, CMB and PTA+Taiji+CE show different parameter degeneracy orientations, and thus the combination of them could effectively break the parameter degeneracies and improve constraint precisions of cosmological parameters. In the $\Lambda$CDM model, the constraint precisions of $\Omega_{\rm m}$ and $H_0$ using the CMB+PTA+Taiji+CE data are better than or at least equal to $1\%$. While in the $w$CDM model, CMB+PTA+Taiji+CE offers $\sigma(w)=0.028$, which is comparable with the latest constraint result by the CMB+BAO+SN data. Compared with CMB, the combination of CMB and PTA+Taiji+CE could improve the constraint on $w$ by $86.7\%$. In the $w_0w_a$CDM model, the CMB+PTA+Taiji+CE data offer $\sigma(w_0)=0.110$ and $\sigma(w_a)=0.32$, which are $81.8\%$ and $87.2\%$ better than the results by CMB.

Hence, we can conclude that: (i) the joint future multi-band GW standard sirens could precisely measure the Hubble constant, but are not good at measuring dark energy; (ii) the joint PTA+Taiji+CE data could effectively break the cosmological parameter degeneracies generated by the CMB data, especially in the dynamical dark energy models. It is worth expecting to use the future multi-band GW observations to probe the nature of dark energy and measure the Hubble constant.

\section*{Acknowledgements}
We thank Tao Han and Peng-Ju Wu for helpful discussions.
This work was supported by the National Key R\&D Program of China (Grants Nos. 2022SKA0110200 and 2022SKA0110203) and the National Natural Science Foundation of China (Grants Nos. 11975072, 11875102, and 11835009).

\section*{Data Availability}
The data underlying this article will be shared on reasonable request
to the corresponding author.

\bibliographystyle{mnras}

redpajama_set_name: RedPajamaArXiv


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The krone (Danish pronunciation: [ˈkʁoːnə]; plural: kroner; sign: kr.; code: DKK) is the official currency of Denmark, Greenland and the Faroe Islands, introduced on 1 January 1875. Both the ISO code "DKK" and currency sign "kr." are in common use; the former precedes the value, the latter in some contexts follows it. The currency is sometimes referred to as the Danish crown in English, since krone literally means crown. Historically, krone coins have been minted in Denmark since the 17th century. One krone is subdivided into 100 øre (Danish pronunciation: [ˈøːɐ]; singular and plural), the name øre possibly deriving from Latin aureus meaning "gold coin". Altogether there are eleven denominations of the krone, with the smallest being the 50 øre coin, which is valued at one half of a krone. Formerly there were more øre coins, but those were discontinued due to inflation. The krone is pegged to the euro via the ERM II, the European Union's exchange rate mechanism. Adoption of the euro is favoured by the major political parties, however a 2000 referendum on joining the Eurozone was defeated with 53.2% voting to maintain the krone and 46.8% voting to join the Eurozone.


The first banners advertising the summer festivals, the panigiria, have been spotted again, signalling the start of the Kythirian summer 2017. Kato Livadi is this year's kick-off: Saturday, July 22nd, from 9pm onwards with live music, dance, food and drinks. Don't miss it because it's great fun to dance the Karavitikos, the Chaniotikos or the Kalamatianos together with enthusiastic Greek islanders. Many other villages will follow: the program is not yet complete, but you can already note these dates in your diary: July 28th Kalokairines, August 6th Avlemonas, August 12th Mitata, August 15th Potamos, August 19th Fratsia, September 15th Kalamos, and September 23rd Agia Pelagia.


ANARCHY | Frank Miller Ink.
For the past couple of years, people have been asking what has happened to Frank Miller. The Sin City and The Dark Knight Returns scribe met disappointment with his take on a young Batman and Robin in All-Star Batman and Robin. He followed that with the recently released critical failure (and utter piece of trash in this blogger's opinion) Holy Terror. The man is completely entitled to his opinion, but he may have definitely put a final nail into the coffin containing a sizable amount of his fandom with talk of the immaturity and aimlessness of the Occupy Wall Street movement. Well, that and he peppered his commentary with more of the bigoted xenophobia found in Holy Terror.
The truth is Frank Miller has had some good story ideas (like the concept behind Batman: Year One and the whole approach to dealing with Silver Age Green Lantern in ASBAR), but he has never been a great writer and has always been insane. My primary issue with Miller's writing is that it always falls back on "might makes right". I'm not familiar with his CV, but I'm pretty sure it doesn't include a run writing for any Spider-Man book or Fantastic Four. But how about a book with Batman laying the smackdown on Superman? How about kicking a dude down a pit? How about shooting off a man's mutated testicles? He's good at that sort of thing. That's solid, immediately gratifying entertainment. That's the kind of mind we're dealing with here.
And as much as I don't care for much of what Frank Miller has done, I'll pay to see Sin City 2 as soon as it comes out in the theater because I like the style. I'm not buying his books, and I'm not even remotely agreeing with his stand on anything. The guy's kind of crazy, so you should expect his work to be uneven and his opinions to be unpleasant.
Stephen Colbert Testifies Before Congress | Indecision Forever | Political Humor, 2010 Election, and Satire Blog | Comedy Central.
I remember reading classic political satire in my high school English classes. We discussed the value of the satirical approach in bringing to light important issues, as well as the subversive nature of the humor sometimes involved. (To be fair, some people fail at it.) The masses receive the satire these days on television. The most popular forms are The Daily Show and The Colbert Report. Some people confuse these shows for real news shows, which is disappointing. They are opinionated and they are quite pointed. More importantly, they point out the flaws, hypocrisies, and stupidity of the people in our political world. I see value in that.
I also see value in Stephen Colbert stepping up the satire and delivering his message in person before Congress. People say that takes chutzpa, but it is easy to have bravado when you have money and supporters behind you. Still, he had a message to deliver and he did so in a memorable way. Whether or not he was taken seriously while he was sitting there, he remained in their heads afterward. Now it is up to them to do something about it.


Full Description: Very nice 3 bedroom, 2 bath manufactured home on a nice sized lot. Open floor plan, new flooring in much of the house, permanent siding, detached 2 car garage. Deck on the back with fenced in yard space. All appliances will stay, f/h, c/a.


Description: Book is bumped and a bit worn at the extremities. One chip/ding at the front spine edge. Pages are free of marks. Binding is tight. Dust jacket has a closed tear with creasing at the lower front fore edge corner. Tiny chips at the corners. Rubbing to surfaces. DJ has been placed in an archival Brodart cover. Part of the Tundra Collection of Children's Books as Works of Art. Copyright 1975. First (English) Edition, 1976.
Size: 8.75 x 10.5 inches.
Pages: Unpaginated. Approx. 32 pages.


text:
Q: How to continuously read from the serial port in Matlab? This is my code:
serialPort = 'COM3';
s = serial(serialPort,'BaudRate',9600);
if (s.Status == 'closed')
    s.BytesAvailableFcnMode = 'byte';
    s.BytesAvailableFcnCount = 200;
    s.BytesAvailableFcn = @Serial_OnDataReceived;

    fopen(s);
end

This is the CallBack function
function Serial_OnDataReceived(obj,event)
global s;
global i;
global endCheck;
global yVals;
global xVals;

if (s.Status == 'open')
    while s.BytesAvailable > 0 && endCheck ~= '1',
        data = str2num(fgetl(s));
        dlmwrite ('SensorsReading.csv', data, '-append');

        yVals = circshift(yVals,-1);
        yVals(end) = data(3);

        xVals = circshift(xVals,-1);
        i = i + 0.0125;
        xVals(end) = i;
    end

    figure(1);
    plot(xVals,yVals);

end

end
Right after the FOPEN function, I get this Warning:

The BytesAvailableFcn is being disabled. To enable the callback property
  either connect to the hardware with FOPEN or set the BytesAvailableFcn property.

Does the logic that happens in the callback function Serial_OnDataReceived run on a different thread?
Is there a way to pass parameters to the function? I want to modify an array in the main script from the callback function, which is in a different file. What's the best way to do so?
I am also trying to plot the values when they're updated to show some kind of dynamic animation.

A: I am not sure about what is generating the warning, but to answer your other question (how to pass parameter to the callback and how to update the plot), a better way to go would be to prepare your plot outside of the callback, then pass the handle to the callback for update only.
nPointsInFigure = 10 ;  %// number of "sliding points" in your figure
step = 0.0125 ;         %// X points spacing
xVals = linspace(-(nPointsInFigure-1)*step,0,nPointsInFigure) ; %// prepare empty data for the plot
yVals = NaN(nPointsInFigure,1) ;

figure(1) ;
hp = plot( xVals , yVals ) ; %// Generate the plot (with empty data) it will be passed to the callback.

serialPort = 'COM3';
s = serial(serialPort,'BaudRate',9600);
if (s.Status == 'closed')
    s.BytesAvailableFcnMode = 'byte';
    s.BytesAvailableFcnCount = 200;
    s.BytesAvailableFcn = {@Serial_OnDataReceived,hp,step} ; %// note how the parameters are passed to the callback
    fopen(s);
end

Your callback will become:
function Serial_OnDataReceived(obj,event,hp,step)

global endCheck; %// I don't know how you use that so I could not get rid of it.

xVals = get(hp,'XData') ; %// retrieve the X values from the plot
yVals = get(hp,'YData') ; %// retrieve the Y values from the plot

while obj.BytesAvailable > 0 && endCheck ~= '1',
    data = str2num(fgetl(s));
    dlmwrite ('SensorsReading.csv', data, '-append');

    yVals = circshift(yVals,-1);
    yVals(end) = data(3);

    xVals = circshift(xVals,-1);
    xVals(end) = xVals(end-1) + step ;
end

set( hp , 'XData',xVals , 'YData',yVals ) ; %// update the plot with the new values

Also note: (1) You don't need to check for the state open/close of the serial port within the callback function. If the event was triggered it means the port was open. (2) you don't need to declare s as global, the obj parameter is actually the serial object itself.

A: If the suggestion from Hoki does not work, try using a timer.
% The following line is useful for debugging
mytimerCallback = @(~, ~) disp('Caught error For Tenzo Timer');

if isempty(timerXbee)
     timerXbee = timer('ExecutionMode','FixedRate','Period',0.1,...
                    'TimerFcn',{@storeDataFromSerial},'ErrorFcn', mytimerCallback);
     try
         start(timerXbee);
     catch
         disp('Timer Xbee');
         disp '******** InstrumentSubscription ERROR *********'
         disp (exception.message);
         disp '***********************************************'
     end
end

% If you are using a polling approach, request data

sendRequest(cmd);
connectionRequested = true;

Then implement the timer function that will be called every period
function storeDataFromSerial(~,~,~)
    while (get(xbee, 'BytesAvailable')~=0)
        serialProtocol();
    end
end

When you want to disconnect the device and close the communication don't forget to stop the timer with
stop(timerXbee)

redpajama_set_name: RedPajamaStackExchange


text:
/*
5
*/
import UnityScript.Tests;

foo = GetComponent(ComponentFoo);
foo.fooFloat += 2;
foo.fooFloat += 3;
print(foo.fooFloat);

redpajama_set_name: RedPajamaGithub


Andrew Robinson marvels at the brain power and breadth of knowledge of the 18th-century polymath Thomas Young. He examines his relationship with his contemporaries, particularly with the French Egyptologist Champollion, and how he has been viewed subsequently by historians.
Nature to him was an open book, whose letters he could read without effort. ... Reflection, refraction, the formation of images by lenses, the mode of operation of the eye, the spectral decomposition and recomposition of the different kinds of light, the invention of the reflecting telescope, the first foundations of colour theory, the elementary theory of the rainbow pass by us in procession, and finally come his observations of the colours of thin films as the origin of the next great theoretical advance, which had to await, over a hundred years, the coming of Thomas Young.


As Mexico moves further through World Cup 2018 qualifying, let's take a look at one player that the opposition will definitely need to keep an eye on: Carlos Vela. The 27-year-old has been playing in the top leagues of Europe for the majority of his career, and now he'll be hoping to help Mexico take another step toward qualifying for their seventh straight World Cup.
Born in Mexico, Vela was almost immediately entrenched into football. After spending time with his local club in Cancún, the winger joined Mexican powerhouse Chivas Guadalajara's youth academy in 2002. He would remain with Guadalajara for just over three years, but would never make a first team appearance.
Due to impressive performances with the Mexican Youth National Team, Vela caught the eye of several European clubs, including Arsenal. The Gunners signed Vela for a reported transfer fee of €1 million during the 2006 Winter Transfer Window. Due to work permit issues, the Mexican would spend his first half season of European football with Celta de Vigo, but once again, he would not make a single appearance for the club.
In what would become a theme for Vela during his time at the Emirates, Arsenal loaned him out once again for the 2006/07 campaign. This time, the teenager was sent to the Spanish second division with Salamanca. His performances with the Charros sparked optimism for Arsenal fans as he became a key part of the Spanish club's attack. He would make 31 appearances for Salamanca, scoring eight goals along the way.
Despite the praise from the boss, Vela would spend the next season on loan once again due to work permit issues. His next stop was to La Liga's Osasuna. While he was unable to replicate his eight-goal tally from the previous season, Vela was still able to make 33 appearances in Spain's top flight while contributing three goals and four assists. Osasuna would narrowly escape relegation that season, finishing just a single point ahead of Real Zaragoza for the final safe spot.
Vela was finally able to join Arsenal's first team for the 2008/09 season. His displays in Spain, and with the Mexican National Team gave Arsenal fans hope that he could become an exciting part of the attack. Things didn't exactly go to plan.
Over the next two-and-a-half seasons, Vela would start just three Premier League matches. Altogether he would end up making only 29 league appearances for the Gunners, but, on the bright side, he was able to make his European debut in the Champions League during the 2008/09 campaign. His most productive match for the Gunners actually came in a two-goal performance against Braga in the historic competition.
After failing to secure a consistent spot in Wenger's first team plans, Vela was once again sent on loan for the second half of the 2010/11 season. West Bromwich Albion represented the latest stop in the Mexican's journey around Europe. In just eight appearances for the Baggies, Vela scored twice, and also assisted one goal.
The next season would prove to be the turning point in Vela's floundering European career as Arsenal sent him on loan to Real Sociedad. Sociedad seemingly provided the spark that the winger so desperately needed as he recorded a career-high in goals (12) and assists (seven). He even managed to score against Barcelona in a narrow 2-1 defeat.
His wish became reality as Sociedad agreed a reported €3 million fee for his services on a permanent basis. Vela almost immediately made that price tag look like a bargain as he somehow managed to improve on his breakthrough campaign the previous year. Out of the team's 38 league matches, Vela would appear in all but three. Once again, he would set new career-highs in goals (14) and assists (nine). His amazing performances helped to push Sociedad all the way to Champions League qualification as they narrowly edged Valencia for the fourth spot in the table.
Sociedad's time in the Champions League was shortlived, however, as they crashed out of the group stage without winning a single match. While they struggled in Europe, Vela thrived domestically. His dynamic performances continued as he started 35 times for the club, and set yet another career-high in goals (16) and assists (12). Against his former club Celta Vigo, the winger pulled out a four-goal night that included this game-winner.
Alongside Antoine Griezmann, Vela and Sociedad looked like a club set for bigger things. Sadly, the French striker left for greener pastures during the 2014 Summer Transfer Window joining Atlético Madrid. So far, things have worked out pretty nicely for him there.
Things have not gone so well for Sociedad. Since Griezmann's departure, Vela has been unable to live up to the heights he met during the previous two seasons. Sociedad haven't finished higher than ninth, and they're currently on their third manager in three seasons.
Vela's time with the Mexican National Team hasn't always been smooth sailing. After leading the U17 National Team to victory in the 2005 World Championships, fans had no reason not to expect the teenager to become a star on the senior level.
He would make his first international appearance during a 2007 friendly against Brazil. His first major tournament for El Tri was the 2009 CONCACAF Golf Cup, but an injury in the opening match forced him out until the semifinals. During that match against Costa Rica, Vela would end up scoring the winning penalty to send Mexico to the finals. In that final match, Mexico absolutely battered the US 5-0, with Vela scoring the third goal of the match.
At the 2010 World Cup in South Africa, Vela would make just two appearances as injuries once again plagued his time with the national side.
Later that year, Vela was handed a six-month ban from the national team for his alleged involvement in a party after a match against Colombia.
Since then, the winger has refused call-ups for the London Olympics and World Cup Qualifying matches. He was also not a part of the 2014 World Cup squad.
In 2015, he returned to international action as a member of the Gold Cup squad. Vela started Mexico's first five matches, but a yellow card suspension ruled him out for the final against Jamaica. Mexico would go on to win the final 3-1.
While he's typically deployed on the right wing, Vela can also line-up as a striker if called upon. When he's in-form, the 27-year-old can be lethal cutting inside from the flanks, and he's proven that he can setup goals for his teammates.